140 research outputs found
Solitonic spin-liquid state due to the violation of the Lifshitz condition in FeTe
A combination of phenomenological analysis and M\"ossbauer spectroscopy
experiments on the tetragonal FeTe system indicates that the magnetic
ordering transition in compounds with higher Fe-excess, 0.11, is
unconventional. Experimentally, a liquid-like magnetic precursor with
quasi-static spin-order is found from significantly broadened M\"ossbauer
spectra at temperatures above the antiferromagnetic transition. The
incommensurate spin-density wave (SDW) order in FeTe is described by a
magnetic free energy that violates the weak Lifshitz condition in the Landau
theory of second-order transitions. The presence of multiple Lifshitz
invariants provides the mechanism to create multidimensional, twisted, and
modulated solitonic phases.Comment: 5 pages, 2 figure
Interplay of magnetism and superconductivity in EuFe(AsP) single crystals probed by muon spin rotation and Fe M\"ossbauer spectroscopy
We present our results of a local probe study on
EuFe(AsP) single crystals with =0.13, 0.19 and
0.28 by means of muon spin rotation and Fe M\"ossbauer spectroscopy.
We focus our discussion on the sample with =0.19 viz. at the optimal
substitution level, where bulk superconductivity ( K) sets in
above static europium order (K) but well below the onset of
the iron antiferromagnetic (AFM) transition (100 K). We find enhanced
spin dynamics in the Fe sublattice closely above and propose
that these are related to enhanced Eu fluctuations due to the evident coupling
of both sublattices observed in our experiments.Comment: Contribution to the 13th International Conference on Muon Spin
Rotation, Relaxation and Resonance (MuSR2014
HI Observations of the Stephan's Quintet
Using the VLA, we have made spectral-line and continuum observations of the
neutral hydrogen in the direction of the compact group of galaxies Stephan's
Quintet. The high-velocity clouds between 5600 and 6600 km/s, the disk of the
foreground galaxy, NGC 7320, at 800 km/s, the extended continuum ridge near the
center of the group, and 3 faint dwarf-like galaxies in the surrounding field
were imaged with C, CS, and D arrays. Four of the HI clouds previously detected
are confirmed. The two largest HI features are coincident with and concentrated
mainly along separate large tidal tails that extend eastward. The most diffuse
of the four clouds is resolved into two clumps, one coincide with tidal
features south of NGC 7318a and the other devoid of any detectable stellar or
Halfa sources. The two compact clouds, along the same line of sight, have peak
emission at luminous infrared and bright Halfa sources probably indicative of
star-forming activity. The total amount of HI detected at high redshifts is ~
10**10Msol. As in previous HI studies of the group, no detectable emission was
measured at the positions of any high-redshift galaxies so that any HI still
bound to their disks must be less than 2.4 x 10**7Msol.Comment: Accepted for publication in AJ and tentatively scheduled for the May
2002 issue. High-resolution ps figures are available at:
http://www.iaa.es/~lourdes/bw/bw-paper.tar.g
Associations of Dwarf Galaxies
Hubble Space Telescope Advanced Cameras for Surveys has been used to
determine accurate distances for 20 galaxies from measurements of the
luminosity of the brightest red giant branch stars. Five associations of dwarf
galaxies that had originally been identified based on strong correlations on
the plane of the sky and in velocity are shown to be equally well correlated in
distance. Two more associations with similar properties have been discovered.
Another association is identified that is suggested to be unbound through tidal
disruption. The associations have the spatial and kinematic properties expected
of bound structures with 1 - 10 x 10^11 solar mass. However, these entities
have little light with the consequence that mass-to-light ratios are in the
range 100 - 1000 in solar units. Within a well surveyed volume extending to 3
Mpc, all but one known galaxy lies within one of the groups or associations
that have been identified.Comment: 50 pages, 2 tables, 15 encapsulated figures, 1 (3 part) jpg figure.
Submitted to Astronomical Journa
Fast recovery of the stripe magnetic order by Mn/Fe substitution in F-doped LaFeAsO superconductors
As Nuclear Magnetic (NMR) and Quadrupolar (NQR) Resonance were used,
together with M\"{o}ssbauer spectroscopy, to investigate the magnetic state
induced by Mn for Fe substitutions in F-doped LaFeMnAsO
superconductors. The results show that % of Mn doping is enough to
suppress the superconducting transition temperature from 27 K to zero and
to recover the magnetic structure observed in the parent undoped LaFeAsO. Also
the tetragonal to orthorhombic transition of the parent compound is recovered
by introducing Mn, as evidenced by a sharp drop of the NQR frequency. The NQR
spectra also show that a charge localization process is at play in the system.
Theoretical calculations using a realistic five-band model show that
correlation-enhanced RKKY exchange interactions between nearby Mn ions
stabilize the observed magnetic order, dominated by and
ordering vectors. These results give compelling evidence that
F-doped LaFeAsO is a strongly correlated electron system at the verge of an
electronic instability.Comment: 5 pages, 5 figures and 4 pages of supplemental materia
The dynamical status of Stephan's Quintet
Multiwavelength data for Stephan's Quintet (SQ) are consistent with the
following model for this compact galaxy group. (1) Discordant redshift NGC 7320
is an unrelated foreground galaxy. (2) In the past SQ was an accordant redshift
quartet involving NGC 7317, 18A, 19 and 20C. NGC 7320C collided (probably not
for the first time) with the group a few times 10 years ago and stripped
the interstellar matter from NGC 7319. (3) In the present SQ is again an
accordant quartet involving NGC 7317, 18A,B, and 19. NGC 7318B is now entering
the group at high velocity for the first time, giving rise to a shock zone. If
most compact groups are like SQ, then they are frequently visited by infalling
n eighbors that perturb the group and themselves. SQ represents strong evidence
for secondary infall in a small group environment. Tidal stripping reduces the
mass of the infalling galaxies, thereby increasing the timescale for their
orbital decay. There is little evidence that these high velocity ``intruders''
are rapidly captured and/or merge with the system. Instead they are the
mechanism that sustains compact groups against collapse. Efficient gas
stripping may account for the low star formation rate observed in compact
groups and infall of residual gas into galactic nuclei may also foster the
onset of AGN activity.Comment: 5 pages, 2x3 figures, to be published in ApJ Letter
Galaxy Distances in the Nearby Universe: Corrections For Peculiar Motions
By correcting the redshift--dependent distances for peculiar motions through
a number of peculiar velocity field models, we recover the true distances of a
wide, all-sky sample of nearby galaxies (~ 6400 galaxies with velocities
cz<5500 km/s), which is complete up to the blue magnitude B=14 mag. Relying on
catalogs of galaxy groups, we treat ~2700 objects as members of galaxy groups
and the remaining objects as field galaxies.
We model the peculiar velocity field using: i) a cluster dipole
reconstruction scheme; ii) a multi--attractor model fitted to the Mark II and
Mark III catalogs of galaxy peculiar velocities. According to Mark III data the
Great Attractor has a smaller influence on local dynamics than previously
believed, whereas the Perseus-Pisces and Shapley superclusters acquire a
specific dynamical role. Remarkably, the Shapley structure, which is found to
account for nearly half the peculiar motion of the Local Group, is placed by
Mark III data closer to the zone of avoidance with respect to its optical
position.
Our multi--attractor model based on Mark III data favors a cosmological
density parameter Omega ~ 0.5 (irrespective of a biasing factor of order
unity). Differences among distance estimates are less pronounced in the ~ 2000
- 4000 km/s distance range than at larger or smaller distances. In the last
regions these differences have a serious impact on the 3D maps of the galaxy
distribution and on the local galaxy density --- on small scales.Comment: 24 pages including (9 eps figures and 7 tables). Figures 1,2,3,4 are
available only upon request. Accepted by Ap
Cepheid Calibration of the Peak Brightness of SNe Ia -- IX. SN 1989B in NGC 3627
(Abridged) Repeated imaging observations have been made of NGC 3627 with the
HST in 1997/98, over an interval of 58 days. Images were obtained on 12 epochs
in the F555W band and on five epochs in the F814W band. The galaxy hosted the
prototypical, `Branch normal', type Ia supernova SN 1989B. A total of 83
variables have been found, of which 68 are definite Cepheid variables with
periods ranging from 75 days to 3.85 days. The de-reddened distance modulus is
determined to be (m-M)_0= 30.22+/-0.12 (internal uncertainty) using a subset of
the Cepheid data whose reddening and error parameters are secure.
The photometric data of Wells et al. (1994), combined with the Cepheid data
for NGC 3627 give M_B(max)= -19.36+/-0.18 and M_V(max)= -19.34+/-0.16 for SN
1989B. Combined with the previous six calibrations in this program, plus two
additional calibrations determined by others gives the mean absolute magnitudes
at maximum of = -19.48+/-0.07 and = -19.48 +/-0.07 for `Branch
normal' SNe Ia at this interim stage in the calibration program.
The second parameter correlations of M(max) of blue SNe Ia with decay rate,
color at maximum, and Hubble type are re-investigated. The dependence of
on decay rate is non-linear, showing a minimum for decay rates between
1.0< Delta m_15 <1.6. Magnitudes corrected for decay rate show no dependence on
Hubble type, but a dependence on color remains. Correcting both the fiducial
sample of 34 SNe Ia with decay-rate data and the current 8 calibrating SNe Ia
for the correlation with decay rate as well as color gives H_0= 60+/-2
(internal) km/s/Mpc, in both B and V. The same value to within 4% is obtained
if only the SNe Ia in spirals (without second parameter corrections) are
considered.Comment: 32 pages (with 7 tables and 14 figures) LaTeX, uses emulateapj.sty; a
full-resolution version with complete figs. 4 and 5 is available at
http://www.astro.unibas.ch/cosmology/papers.html ; accepted for publication
in Ap
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