arXiv subjects

Tereasa G. Brainerd

Publications and source records attributed to Tereasa G. Brainerd.

27 records · Page 2Linked to original sources

arXiv2004

Concordance between the Dynamics of Satellite Galaxies in the 2dFGRS and Lambda-CDM

We compute the velocity dispersion profile, \sigmav(r_p), for satellites of host galaxies in the Two Degree Field Galaxy Redshift Survey (2dFGRS) and in the Lambda-CDM GIF simulation. We find 1345 hosts in the 2dFGRS with luminosities in the range 0.5 L* < L < 5.5 L*, for which a total of 2475 satellite galaxies is obtained. The magnitudes of the galaxies in the GIF simulation are converted to the b_J band pass, and hosts and satellites are selected in the same manner as in the 2dFGRS. Of order 1200 hosts and 4100 satellites are found in the simulation. Overall, there is excellent agreement between \sigmav(r_p) for the satellites in the 2dFGRS and the GIF simulation. On large scales, \sigmav(r_p) decreases with projected radius, in good agreement with the expectations of a CDM universe. Further, there is a marked dependence of \sigmav(r_p) on both the host spectral type and the host luminosity. In particular, \sigmav(r_p) has a substantially higher amplitude and steeper slope for satellites of early-type hosts than it does for satellites of late-type hosts. In addition, both the amplitude and slope of \sigmav(r_p) increase with host luminosity. The velocity dispersion of satellites located within small projected radii (r_p < 120 kpc) is only marginally consistent with the local B-band Tully-Fisher relation, and is fitted best by a relationship of the form σ_v \propto L^{0.45 \pm 0.10}.

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arXiv2004

The Effects of Multiple Weak Deflections in Galaxy-Galaxy Lensing

The Hubble Deep Field (North) and the flanking fields are used investigate the occurrence of multiple weak lensing deflections along the line of sight in relatively deep imaging data (z_lens ~ 0.6, z_source ~ 1.2). Ray tracing simulations of galaxy-galaxy lensing in the HDF-North show that proper inclusion of multiple weak deflections is important for a correct prediction of the net shear for most sources, and for a given source redshift the number of multiple weak deflections is largely insensitive to the cosmography. The effects of multiple weak deflections on the magnitude of the weak lensing signal are, of course, strong functions of the adopted halo parameters. Independent of the halo parameters, however, the closest lens to a source (in projection on the sky) is not the strongest lens in the case of more than 50% of the sources which acquire a net shear of γ< 0.01. In addition, multiple weak deflections result in a tangential shear about the lens centers that is greater than the tangential shear that would occur if source galaxies were lensed solely by the closest lens. Further, multiple weak deflections give rise to correlated image ellipticities and account for a substantial amount of the total cosmic shear signal on small angular scales in Lambda-CDM and open CDM models.

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arXiv2003

Mass-to-Light Ratios of 2dF Galaxies

We compute M_260, the dynamical mass interior to a radius of 260 kpc/h, for a set of 809 isolated host galaxies in the 100k data release of the 2dF Galaxy Redshift Survey. The hosts are surrounded by 1556 satellite galaxies, as defined by a set of specific selection criteria. Our mass estimator and host/satellite selection criteria are taken from those used by the Sloan Digital Sky Survey (SDSS) collaboration for an analysis of M_260 for SDSS galaxies and, overall, our results compare well with theirs. For L > 2L* we find M_260/L = (193 +/- 14)h Msun/Lsun, with a tendency for hosts with L < 2L* to have a somewhat higher M/L. We also investigate M/L seperately for bright galaxies with ellipitical, S0, and spiral morphologies. There are 159 hosts in the elliptical/S0 sample, for which we find M_260/L = (271 +/- 26) h Msun/Lsun for galaxies with L > 2L*, and a weak tendency for intrinsically fainter galaxies to have a somewhat higher M/L. In stark contrast to this, we find the line of sight velocity dispersion for the 243 spiral hosts to be independent of the host galaxy luminosity, yielding a value of sigma_v = 189 +/- 19 km/s. Thus for the spiral hosts, M_260/L is proportional to L^{-1.0 +/- 0.2}, and we find M_260/L for a 2L* spiral is of order 200 h Msun/Lsun.

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arXiv1999

Gravitational Lensing by NFW Halos

We investigate the gravitational lensing properties of dark matter halos with Navarro, Frenk & White (NFW) density profiles and derive an analytic expression for the radial dependence of the shear, $γ(x)$, due to these objects. In addition, we derive an expression for the mean shear interior to a given radius, $\barγ(x)$, and use this to quantify systematic errors that will arise in weak lensing mass estimates of astronomical objects in the case that the mass estimate is based on an a priori assumption that the underlying potential is that of a singular isothermal sphere when, in fact, the potential is that of an NFW-type object. On mass scales between $10^{11} \Msun \ls M_{200} \ls 10^{15} \Msun$, the assumption of an isothermal sphere potential results in an overestimate of the halo mass, and the amount by which the mass is overestimated increases linearly with the value of the NFW concentration parameter. Considerable overestimates of the mass ($\sim 60%$) can occur for galaxy-sized halos, but for rich clusters the mass overestimate is small. The degree to which the mass is systematically in error is dependent upon the cosmology adopted, with a COBE-normalized standard CDM model yielding the largest systematic errors for a given true value of the halo mass.

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arXiv1999

The Clustering of Faint Galaxies on Small Angular Scales

We present a preliminary measurement of the angular clustering of faint ($R \le 25$) field galaxies in which we concentrate on the behavior of $w(θ)$ on small angular scales ($θ\ls 10''$). The galaxies are strongly clustered and $w(θ)$ is well-characterized by a power law of the form $A_w θ^{-δ}$. The best-fitting value of the power law index, $δ$, is, however, steeper than the fiducial value of $δ= 0.8$, indicating there are more pairs of galaxies separated by $θ\ls 10''$ in our sample than would be otherwise expected. Using the best-fitting form of $w(θ)$, we estimate that $\sim 10%$ of the galaxies are in physically close pairs (separations $\ls 21 h^{-1}$ kpc). This is a factor of order 2 larger than local galaxy samples, but comparable to galaxy samples with $ \sim 0.4$. The mean redshift of our galaxies is of order 0.95, and, therefore, our result suggests that there was little or no evolution in the merger rate of galaxies between $z \sim 1$ and $z \sim 0.4$.

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arXiv1999

A Comparison of Simple Mass Estimators for Galaxy Clusters

High-resolution N-body simulations are used to investigate systematic trends in the mass profiles and total masses of clusters as derived from 3 simple estimators: (1) the weak gravitational lensing shear field under the assumption of an isothermal cluster potential, (2) the dynamical mass obtained from the measured velocity dispersion under the assumption of an isothermal cluster potential, and (3) the classical virial estimator. The clusters consist of order 2.5e+05 particles of mass $m_p \simeq 10^{10} \Msun$, have triaxial mass distributions, and significant substructure exists within their virial radii. Not surprisingly, the level of agreement between the mass profiles obtained from the various estimators and the actual mass profiles is found to be scale-dependent. The virial estimator yields a good measurement of the total cluster mass, though it is systematically underestimated by of order 10%. This result suggests that, at least in the limit of ideal data, the virial estimator is quite robust to deviations from pure spherical symmetry and the presence of substructure. The dynamical mass estimate based upon a measurement of the cluster velocity dispersion and an assumption of an isothermal potential yields a poor measurement of the total mass. The weak lensing estimate yields a very good measurement of the total mass, provided the mean shear used to determine the equivalent cluster velocity dispersion is computed from an average of the lensing signal over the entire cluster (i.e. the mean shear is computed interior to the virial radius). [abridged]

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arXiv1997

A Constant Clustering Amplitude for Faint Galaxies?

The angular clustering of faint field galaxies is investigated using deep imaging (I~25) obtained with the 10-m Keck-I telescope. The autocorrelation function is consistent with w(theta) ~ theta^-0.8 and, although less steep correlation functions cannot be ruled out with high confidence, we find no compelling evidence for a systematic decrease in the power law index at the faintest magnitude limits. Results from a number of independent observational studies are combined in order to investigate the variation of the correlation amplitude with median I-magnitude. At Imed~23 the results obtained by different studies are all in rough agreement and indicate that for Imed > 22 the correlation amplitude declines far less steeply than would be expected from an extrapolation of the trend in the brighter samples. In particular, at Imed~24 our data indicate w(theta) to be a factor ~7 higher than the extrapolation. A near-independence of magnitude is a general feature of the correlation amplitude in models in which the redshift distribution of the faint field population contains a substantial fraction of galaxies with z > 1. In order to reproduce the apparent abrupt flattening of the amplitude of w(theta) observed at faint limits, approximately 50% of the galaxies in a sample with a depth of I~25 must be at z > 1.

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arXiv1997

High-Resolution Simulations of Cluster Formation

The formation history of rich clusters is investigated using a hybrid N-body simulation in which high spatial and mass resolution can be achieved self-consistently within a small region of a very large volume. The evolution of three massive clusters is studied via mass accretion, spherically-averaged density profiles, three-dimensional and projected shapes, and degree of substructure. Each cluster consists of order $4\times 10^5$ particles at the present epoch and in the case that rich cluster evolution is well-described by a 1-parameter family, the simulations have sufficient resolution to demonstrate this. At $z=0$ the clusters have similar masses, $M(r \le 1.5h^{-1} Mpc) \sim 2\times 10^{15} h^{-1} M_\odot$, and similar spherically-averaged density profiles, however markedly different formation histories are observed. No single, dominant pattern is apparent in the time variation of the mass accretion rate, the cluster shape, or the degree of substructure. Although not a statistically large sample, these objects suggest that the detailed formation history of rich clusters cannot be characterized by a simple 1-parameter family. These results suggest that the use of observations of rich clusters over a wide range of redshifts to constrain cosmological parameters may not be entirely straightforward.

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arXiv1994

Evolution in the Clustering of Galaxies to r = 26 (TAPIR GRP-390)

We present results for the two-point angular correlation function of galaxies to a limiting magnitude of r=26. The final sample is 97% complete to r=26.0, yielding 5730 galaxies over a 90.1 sq. arcmin field. The correlation function for our faint galaxies can be parameterised by a power law, $A θ^{-0.8}$, in agreement with the clustering statistics of shallower catalogues. The derived amplitude, $A$, is small, but non-zero. We combine this measurement with the latest statistical constraints on faint galaxy redshifts from gravitational lensing studies, which imply that the bulk of the r<26 field galaxies should be at redshifts of order 1. Our derived $A$ is significantly lower than that predicted from the local bright galaxy correlation function using the lensing-determined galaxy redshift distribution and modest growth of clustering. This simplistic model does not include the variation in observed morphological mix as a function of redshift and apparent magnitude in our sample. At our faintest limits we reach sufficiently high redshifts that differential $K$ corrections will result in the observed galaxy mix being dominated by star bursting dwarf and low surface brightness irregulars, rather than the early-type systems used to define the local bright galaxy correlation function. Adopting the correlation function measured locally for these low surface brightness galaxies and assuming modest clustering evolution, we obtain reasonable agreement between our model and observations. This model supports the scenario in which the high number density of faint galaxies is produced by normally clustered star forming dwarf galaxies at modest redshifts.

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