arXiv subjects

M. Sawicki

Publications and source records attributed to M. Sawicki.

At least 91 records · Page 5Linked to original sources

arXiv2005

Prospects of high temperature ferromagnetism in (Ga,Mn)As semiconductors

We report on a comprehensive combined experimental and theoretical study of Curie temperature trends in (Ga,Mn)As ferromagnetic semiconductors. Broad agreement between theoretical expectations and measured data allows us to conclude that T_c in high-quality metallic samples increases linearly with the number of uncompensated local moments on Mn_Ga acceptors, with no sign of saturation. Room temperature ferromagnetism is expected for a 10% concentration of these local moments. Our magnetotransport and magnetization data are consistnent with the picture in which Mn impurities incorporated during growth at interstitial Mn_I positions act as double-donors and compensate neighboring Mn_Ga local moments because of strong near-neighbor Mn_Ga-Mn_I antiferromagnetic coupling. These defects can be efficiently removed by post-growth annealing. Our analysis suggests that there is no fundamental obstacle to substitutional Mn_Ga doping in high-quality materials beyond our current maximum level of 6.2%, although this achievement will require further advances in growth condition control. Modest charge compensation does not limit the maximum Curie temperature possible in ferromagnetic semiconductors based on (Ga,Mn)As.

cond-mat.mtrl-sci↗

arXiv2004

Magnetism in (Ga,Mn)As Thin Films With TC Up To 173K

We have investigated the magnetic properties of (Ga,Mn)As thin films with Mn concentration between 1 and 9%. Ferromagnetic transition temperatures TC of up to 173K are observed. The results are compared to the predictions of the Zener mean-field theory. We find no evidence of a fundamental limit to TC.

cond-mat.str-el↗

arXiv2004

MnAs overlayer on GaN(0001)-(1x1) - its growth, morphology and electronic structure

Spontaneous formation of grains has been observed for the MnAs layer grown by means of MBE on the GaN(0001)-(1x1) surface. Electronic structure of the system was investigated in situ by resonant photoemission spectroscopy. Density of the valence band states of MnAs and its changes due to increase of the layer thickness were revealed.

cond-mat.mtrl-sci↗

arXiv2004

Search For Hole Mediated Ferromagnetism In Cubic (Ga,Mn)N

Results of magnetisation measurements on p-type zincblende-(Ga,Mn)N are reported. In addition to a small high temperature ferromagnetic signal, we detect ferromagnetic correlation among the remaining Mn ions, which we assign to the onset of hole-mediated ferromagnetism in (Ga,Mn)N.

cond-mat.mtrl-sci↗

arXiv2004

In-plane uniaxial anisotropy rotations in (Ga,Mn)As thin films

We show, by SQUID magnetometry, that in (Ga,Mn)As films the in-plane uniaxial magnetic easy axis is consistently associated with particular crystallographic directions and that it can be rotated from the [-110] direction to the [110] direction by low temperature annealing. We show that this behavior is hole-density-dependent and does not originate from surface anisotropy. The presence of uniaxial anisotropy as well its dependence on the hole-concentration and temperature can be explained in terms of the p-d Zener model of the ferromagnetism assuming a small trigonal distortion.

cond-mat.mtrl-sci↗

arXiv2003

Mn Interstitial Diffusion in (Ga,Mn)As

We present a combined theoretical and experimental study of the ferromagnetic semiconductor (Ga,Mn)As which explains the remarkably large changes observed on low temperature annealing. Careful control of the annealing conditions allows us to obtain samples with ferromagnetic transition temperatures up to 159 K. Ab initio calculations, and resistivity measurements during annealing, show that the observed changes are due to out-diffusion of Mn interstitials towards the surface, governed by an energy barrier of about 0.7-0.8 eV. The Mn interstitial is a double donor resulting in compensation of charge carriers and suppression of ferromagnetism. Electric fields induced by high concentrations of substitutional Mn acceptors have a significant effect on the diffusion.

cond-mat.mtrl-sci↗

arXiv2003

Probing hole-induced ferromagnetic exchange in magnetic semiconductors by inelastic neutron scattering

The effect of hole doping on the exchange coupling of the nearest neighbor (NN) Mn pairs in Zn$_{1-x}$Mn$_x$Te is probed by inelastic neutron scattering. The difference in the NN exchange energy $ΔJ_1$ in the presence and in the absence of the holes is determined. The obtained value of $ΔJ_1$ is in good agreement with the predictions of the Zener/RKKY model, even on the insulator side of the metal-insulator transition.

cond-mat.mtrl-sci↗

arXiv2002

Temperature Dependent Magnetic Anisotropy in (Ga,Ma)As Layers

It is demonstrated by SQUID magnetization measurements that (Ga,Mn)As films can exhibit rich characteristics of magnetic anisotropy depending not only to the epitaxial strain but being strongly influenced by the hole and Mn concentration, and temperature. This behavior reflects the spin anisotropy of the valence subbands and corroborates predictions of the mean field Zener model of the carrier mediated ferromagnetism in III-V diluted magnetic semiconductors with Mn. At the same time the existence of in-plane uniaxial anisotropy with [110] the easy axis is evidenced. This is related to the top/bottom symmetry breaking, resulting in the lowering of point symmetry of (Ga,Mn)As to the C_{2v} symmetry group. The latter mechanism coexists with the hole-induced cubic anisotropy, but takes over close to T_C.

cond-mat.mtrl-sci↗

arXiv2001

Dynamically Close Galaxy Pairs and Merger Rate Evolution in the CNOC2 Redshift Survey

We investigate redshift evolution in the galaxy merger and accretion rates, using a well-defined sample of 4184 galaxies with 0.12 < z < 0.55 and R_C < 21.5. We identify 88 galaxies in close (5 < r_p < 20 h^{-1} kpc) dynamical (delta v < 500 km/s) pairs. These galaxies are used to compute global pair statistics, after accounting for selection effects resulting from the flux limit, k-corrections, luminosity evolution, and spectroscopic incompleteness. We find that the number of companions per galaxy (for -21 < M_B^{k,e} < -18) is Nc = 0.0321 +/- 0.0077 at z=0.3. The luminosity in companions, per galaxy, is Lc = 0.0294 +/- 0.0084 x 10^10 h^2 L_sun. We assume that Nc is proportional to the galaxy merger rate, while Lc is directly related to the mass accretion rate. After increasing the maximum pair separation to 50 h^{-1} kpc, and comparing with the low redshift SSRS2 pairs sample, we infer evolution in the galaxy merger and accretion rates of (1+z)^{2.3 +/- 0.7} and (1+z)^{2.3 +/- 0.9} respectively. These are the first such estimates to be made using only confirmed dynamical pairs. When combined with several additional assumptions, this implies that approximately 15% of present epoch galaxies with -21 < M_B < -18 have undergone a major merger since z=1.

astro-ph↗

arXiv2001

Environment and Galaxy Evolution at Intermediate Redshift in the CNOC2 Survey

(abridged) The systematic variation of galaxy colors and types with clustering environment could either be the result of local conditions at formation or subsequent environmental effects as larger scale structures draw together galaxies whose stellar mass is largely in place. At z~0.4 the co-moving galaxy correlation length, r_0, measured in the CNOC2 sample is strongly color dependent, rising from 2/h Mpc to nearly 10/h Mpc as the volume-limited subsamples range from blue to red. The luminosity dependence of r_0 at z~0.4 is weak below L_ast although there is an upturn at high luminosity where its interpretation depends on separating it from the r_0-color relation. The dominant effect of the group environment on star formation is seen in the radial gradient of the mean galaxy colors which on the average become redder than the field toward the group centers. The redder-than-field trend applies to groups with a line-of-sight velocity dispersion, sigma_1>150 kms. There is an indication, somewhat statistically insecure, that the high luminosity galaxies in groups with sigma_1<125 kms become bluer toward the group center. We conclude that the higher velocity dispersion groups largely act to suppress star formation relative to the less clustered field, leading to ``embalmed'' galaxies. The tidal fields within the groups appear to be a strong candidate for the physical source of the reduction of star formation in group galaxies relative to field. Tides operate effectively at all velocity dispersions to remove gas rich companions and low density gas in galactic halos. Given that much of the field population is in groups we suggest that this suppression may be the dominant galaxy evolution force at low redshift.

astro-ph↗

arXiv2001

The Galaxy Correlation Function in the CNOC2 Redshift Survey: Dependence on Color, Luminosity and Redshift

We examine how the spatial correlation function of galaxies from the CNOC2 Field Galaxy Redshift Survey depends on galaxy color, luminosity and redshift. The projected correlation function w_p is determined for volume-limited samples of objects with 0.12 < z < 0.51 and evolution-compensated Rc absolute magnitudes M < -20, over the comoving projected separation range 0.04 Mpc/h < r_p < 10 Mpc/h. Our sample consists of 2937 galaxies which are classified as being either early- or late-type objects according to their spectral energy distribution (SED), determined from UBVRcIc photometry. For simplicity, galaxy SEDs are classified independently of redshift: our classification scheme therefore does not take into account the colour evolution of galaxies.

astro-ph↗

arXiv2000

Weak lensing study of low mass galaxy groups: implications for Omega_m

We report on the first measurement of the average mass and mass-to-light ratio of galaxy groups by analysing the weak lensing signal induced by these systems. The groups, which have velocity dispersions of 50-400 km/s, have been selected from the Canadian Network for Observational Cosmology Field Galaxy Redshift Survey (CNOC2). This survey allows the identification of a large number of groups with redshifts ranging from z=0.12-0.55, ideal for a weak lensing analysis of their mass distribution. For our analysis we use a sample of 50 groups which are selected on the basis of a careful dynamical analysis of group candidates. We detect a signal at the 99% confidence limit. The best fit singular isothermal sphere model yields an Einstein radius of 0.72+-0.29". This corresponds to a velocity dispersion of 274^{+48}_{-59} km/s (using photometric redshift distributions for the source galaxies), which is in good agreement with the dynamical estimate. Under the assumption that the light traces the mass, we find an average mass-to-light ratio of 191+-83 h Msun/Lsun in the restframe B band. Unlike dynamical estimates, this result is insensitive to problems associated with determining group membership. After correction of the observed mass-to-light ratio for luminosity evolution to z=0, we find 254+-110 h Msun/Lsun, lower than what is found for rich clusters. We use the observed mass-to-light ratio to estimate the matter density of the universe, for which we find Omega_m=0.19+-0.10 (Omega_Lambda=0), in good agreement with other recent estimates. For a closed universe, we obtain Omega_m=0.13+-0.07.

astro-ph↗

arXiv2000

Galaxy Groups at Intermediate Redshift

Galaxy groups likely to be virialized are identified within the CNOC2 intermediate redshift galaxy survey using an iterative method. The number-velocity dispersion relation is in agreement with the low-mass extrapolation of the cluster normalized Press-Schechter function. The two-point group-group correlation function has r_0=6.8+/- 0.3 Mpc, which is larger than the correlations of individual galaxies at the level predicted from n-body calibrated halo clustering. The groups are stacked in velocity and position to create a sample large enough for measurement of a density and velocity dispersion profile. The stacked mean galaxy density profile falls nearly as a power law with r^{-2.5} and has no well-defined core. The projected velocity dispersion is examined for a variety of samples with different methods and found to be either flat or slowly rising outwards. The combination of a steeper-than-isothermal density profile and the outward rising velocity dispersion implies that the mass-to-light ratio of groups rises with radius. The M/L can be kept nearly constant if the galaxy orbits are nearly circular, although such strong tangential anisotropy is not supported by other evidence. The segregation of mass and light is not dependent on galaxy luminosity but is far more prominent in the red galaxies than the blue. The M/L gradient could arise from orbital ``sloshing'' of the galaxies in the group halos, dynamical friction acting on the galaxies in a background of ``classical'' collisionless dark matter, or, more speculatively, the dark matter may have a true core.

astro-ph↗

arXiv2000

Galaxy Clustering Evolution in the CNOC2 High-Luminosity Sample

The redshift evolution of the galaxy two-point correlation function is a fundamental cosmological statistic. To identify similar galaxy populations at different redshifts, we select a strict volume-limited sample culled from the 6100 cataloged CNOC2 galaxies. Our high-luminosity subsample selects galaxies having k-corrected and evolution-compensated R luminosities, M_R^{k,e}, above -20 mag (H_0=100 km/s/Mpc) where M_ast^{k,e}(R)simeq -20.3 mag. This subsample contains about 2300 galaxies distributed between redshifts 0.1 and 0.65 spread over a total of 1.55 square degrees of sky. A similarly defined low-redshift sample is drawn from the Las Campanas Redshift Survey. We find that the co-moving two-point correlation function can be described as xi(r|z) = (r_00/r)^gamma (1+z)^{-(3+epsilon-gamma)} with r_{00}=5.03+/-0.08/h Mpc, epsilon=-0.17+/- 0.18 and gamma=1.87+/-0.07 over the z=0.03 to 0.65 redshift range, for Omega_M=0.2, Lambda=0. The measured clustering amplitude and its evolution are dependent on the adopted cosmology. The measured evolution rates for Omega_M=1 and flat Omega_M=0.2 background cosmologies are epsilon=0.80+/-0.22 and epsilon=-0.81+/-0.19, respectively, with r_{00} of 5.30+/-0.1/h Mpc and 4.85+/-0.1/h Mpc, respectively. The sensitivity of the derived correlations to the evolution corrections and details of the measurements is presented. The analytic prediction of biased clustering evolution for only the low density, LambdaCDM cosmology is readily consistent with the observations, with biased clustering in an open cosmology somewhat marginally excluded and a biased Omega_M=1 model predicting clustering evolution that is more than 6 standard deviations from the measured value.

astro-ph↗

arXiv2000

The CNOC2 Field Galaxy Redshift Survey I: The Survey and the Catalog for the Patch CNOC 0223+00

The Canadian Network for Observational Cosmology (CNOC2) Field Galaxy Redshift Survey is a spectroscopic/photometric survey of faint galaxies over 1.5 square degrees of sky with a nominal spectroscopic limit of R_c=21.5 mag. The primary goals of the survey are to investigate the evolution of galaxy clustering and galaxy populations over the redshift range of approximately 0.1 to 0.6. The survey area contains four widely separated patches on the sky with a total spectroscopic sample of over 6000 redshifts and a photometric sample of over 40,000 galaxies with 5-color photometry. We describe the survey and observational strategies, multi-object spectroscopy mask design procedure, and data reduction techniques for creating the spectroscopic-photometric catalogs. We also discuss the derivations of various statistical weights for the redshift sample which allow it to be used as a complete sample. As the initial release of the survey data, we present the data set and some statistics for the Patch CNOC0223+00.

astro-ph↗

arXiv1999

Galaxy Clustering in the CNOC2 Redshift Survey

The correlation evolution of a high luminosity subsample of the CNOC2 redshift survey is examined. The sample is restricted to galaxies for which the k corrected and evolution corrected R luminosity is M_R <=-20 mag, where M_* ~= -20.3 mag. This subsample contains about 2300 galaxies. In consort with 13000 galaxies in a similarly defined low redshift sample from the Las Campanas Redshift survey we find that the comoving correlation can be described as xi(r|z) = (r_00/r)^gamma (1+z)^{-(3+e)} with r_00=5.08 +/- 0.08/h Mpc, e=0.02 +/- 0.23 and gamma=1.81 +/- 0.03 over the z=0.03 to 0.65 redshift range in a cosmology with Omega_M=0.2, Lambda=0. The measured clustering amplitude, and its evolution, are dependent on the adopted cosmology. The evolution rates for Omega_M=1 and flat low density models are e=0.9 +/- 0.3 and e=-0.5 +/- 0.2, respectively, with r_00 ~= 5/h Mpc in all cases.

astro-ph↗

arXiv1999

The CNOC2 Field Galaxy Luminosity Function I: A Description of Luminosity Function Evolution

We examine the evolution of the galaxy luminosity function (LF) using a sample of over 2000 galaxies, with 0.12 < z < 0.55 and 17.0 < Rc < 21.5, drawn from the Canadian Network for Observational Cosmology Field Galaxy Redshift Survey (CNOC2), at present the largest such sample at intermediate redshifts. We use UBVRcIc photometry to classify our galaxies into early, intermediate, and late types, for which we compute luminosity functions in the rest-frame B, Rc, and U bandpasses. In particular, we adopt a parameterization of LF evolution including luminosity and number density evolution, and take care to quantify correlations among our LF evolution parameters. Our principal result is a clear quantitative separation of luminosity and density evolution for different galaxy populations, and the finding that the character of the LF evolution is strongly dependent on galaxy type. Specifically, the early- and intermediate-type LF's show primarily brightening at higher redshifts and only modest density evolution, while the late-type LF is best fit by strong number density increases at higher z, with little luminosity evolution. We also carefully measure and account for sample selection effects as functions of galaxy magnitude and color, and show that our results are not significantly affected by potential systematic effects, such as surface brightness selection, photometric errors, or redshift incompleteness. (abstract abridged)

astro-ph↗

arXiv1998

The CNOC2 Field Galaxy Redshift Survey

The CNOC2 field galaxy redshift survey is designed to provide measurements of the evolution of galaxies and their clustering over the redshift range 0 to 0.7. The sample is spread over four sky patches with a total area of about 1.5 square degrees. Here we report preliminary results based on two of the sky patches, and the redshift range of 0.15 to 0.55. We find that galaxy evolution can be statistically described as nearly pure luminosity evolution of early and intermediate SED types, and nearly pure density evolution of the late SED types. The correlation of blue galaxies relative to red galaxies is similar on large scales but drops by a factor of three on scales less than about 0.3/h mpc, approximately the mean scale of virialization. There is a clear, but small, 60%, change in clustering with 1.4 mag of luminosity. To minimize these population effects in our measurement of clustering evolution, we choose galaxies with M_r^{k,e}<= -20 mag as a population whose members are most likely to be conserved with redshift. Remarkably, the evolution of the clustered density in proper co-ordinates at r < 10/h Mpc, proportional to r_0^gamma (1+z)^3, is best described as a ``de-clustering'', (1+z)^{0.6+/-0.4}. Or equivalently, there is a weak growth of clustering in co-moving co-ordinates, x_0~ (1+z)^{-0.3 +/- 0.2}. This conclusion is supported by the pairwise peculiar velocities which rise slightly, but not significantly, into the past. The Cosmic Virial Theorem applied to the CNOC2 data gives Q Omega_M/b=0.11 +/- 0.04$, where Q is the three point correlation parameter and b the bias. Similarly, galaxy groups have a virial mass-to-light ratio (evolution corrected) of M_{virial}/L_R^{k,e} = 215h Lsun/Msun, or Omega_M=0.15 +/- 0.05.

astro-ph↗