212 research outputs found
Close pairs of galaxies with different activity levels
We selected and studied 180 pairs with dV < 800 km/s and Dp < 60 kpc
containing Markarian (MRK) galaxies to investigate the dependence of galaxies'
integral parameters, star-formation (SF) and active galactic nuclei (AGN)
properties on kinematics of pairs, their structure and large-scale
environments. Projected radial separation Dp and perturbation level P are
better measures of interaction strength than dV. The latter correlates with the
density of large-scale environment and with the morphologies of galaxies. Both
galaxies in a pair are of the same nature, the only difference is that MRK
galaxies are usually righter than their neighbors. Specific star formation
rates (SSFR) of galaxies in pairs with smaller Dp or dV is in average 0.5 dex
higher than that of galaxies in pairs with larger Dp or dV. Closeness of a
neighbor with the same and later morphological type increases the SSFR, while
earlier-type neighbors do not increase SSFR. Major interactions/mergers trigger
SF and AGN more effectively than minor ones. The fraction of AGNs is higher in
more perturbed pairs and pairs with smaller Dp. AGNs typically are in stronger
interacting systems than star-forming and passive galaxies. There are
correlations of both SSFRs and spectral properties of nuclei between pair
members.Comment: 4 pages, 3 figures. arXiv admin note: substantial text overlap with
arXiv:1310.024
Close neighbors of Markarian galaxies. II. Statistics and discussions
According to the database from the first paper, we select 180 pairs with dV <
800 km/s and Dp < 60 kpc containing Markarian (MRK) galaxies. We study the
dependence of galaxies integral parameters, star-formation (SF) and active
galactic nuclei (AGN) properties on kinematics of pairs, their structure and
large-scale environments. Following main results were obtained: projected
radial separation Dp between galaxies correlates with the perturbation level P
of the pairs. Both parameters do not correlate with line-of-sight velocity
difference dV of galaxies. Dp and P are better measures of interaction strength
than dV. The latter correlates with the density of large-scale environment and
with the morphologies of galaxies. Both galaxies in a pair are of the same
nature, the only difference is that MRK galaxies are usually brighter than
their neighbors in average by 0.9 mag. Specific star formation rates (SSFR) of
galaxies in pairs with smaller Dp or dV is in average 0.5 dex higher than that
of galaxies in pairs with larger Dp or dV. Closeness of a neighbor with the
same and later morphological type increases the SSFR, while earlier-type
neighbors do not increase SSFR. Major interactions/mergers trigger SF and AGN
more effectively than minor ones. The fraction of AGNs is higher in more
perturbed pairs and pairs with smaller Dp. AGNs typically are in stronger
interacting systems than star-forming and passive galaxies. There are
correlations of both SSFRs and spectral properties of nuclei between pair
members.Comment: 13 pages, 8 figures, 2 table
Influence of ozone therapy on oral tissue in modeling of chronic recurrent aphthous stomatitis
Chronic recurrent aphthous stomatitis (CRAS) belongs to the
group of chronic, inflammatory, ulcerative diseases of the oral mucosa. The aim of this study was to determine the effects of ozone on the morphofunctional peculiarities of the soft tissues in modeling chronic recurrent aphthous stomatitis.
We performed experimental investigation for study of the morpho-functional state of tissues of the oral mucosa in CRAS with using of previously proposed and widely used modeling scheme with ovalbumin and aluminum hydroxide. Two groups of animals were formed (Dutch rabbits, males, aging three-month, weighting 2-2.4 kg). Group of 8 animals with obtained mucosal changes was our comparison group. Other group of 8 animals with obtained mucosal changes was treated by ozone therapy.
Histological investigation has been performed. Microscopical examination of tissue had shown that ozone therapy reduces inflammation and edema and is useful in wound healing in soft tissue as disappearance of necrobiotic processes, epithelialization of aphthous defect, growth of akantotic bands, pronounced
reducing of inflammatory cells and changing of cellular ratio (with of neutrophils part from 38.30Β±2.46% to 6.34Β±0.63%, eosinophils from 5.49Β±0.23% to 2.87Β±0.05%), restoration of the cellular layers of the epithelium, moderately pronounced sclerosis of the papillary layer of the lamina propria. Described results allow to conclude that correction of tissual changes in chronic
recurrent aphthous stomatitis could be obtained with ozone therapy using.
Π₯ΡΠΎΠ½ΠΈΡΠ΅ΡΠΊΠΈΠΉ ΡΠ΅ΡΠΈΠ΄ΠΈΠ²ΠΈΡΡΡΡΠΈΠΉ Π°ΡΡΠΎΠ·Π½ΡΠΉ ΡΡΠΎΠΌΠ°ΡΠΈΡ (Π₯Π ΠΠ‘) ΠΎΡΠ½ΠΎΡΠΈΡΡΡ ΠΊ Π³ΡΡΠΏΠΏΠ΅ Ρ
ΡΠΎΠ½ΠΈΡΠ΅ΡΠΊΠΈΡ
, Π²ΠΎΡΠΏΠ°Π»ΠΈΡΠ΅Π»ΡΠ½ΡΡ
, ΡΠ·Π²Π΅Π½Π½ΡΡ
Π·Π°Π±ΠΎΠ»Π΅Π²Π°Π½ΠΈΠΉ ΡΠ»ΠΈΠ·ΠΈΡΡΠΎΠΉ ΠΎΠ±ΠΎΠ»ΠΎΡΠΊΠΈ ΠΏΠΎΠ»ΠΎΡΡΠΈ ΡΡΠ°.
Π¦Π΅Π»ΡΡ ΠΈΡΡΠ»Π΅Π΄ΠΎΠ²Π°Π½ΠΈΡ ΡΠ²ΠΈΠ»ΠΎΡΡ ΠΎΠΏΡΠ΅Π΄Π΅Π»Π΅Π½ΠΈΠ΅ Π²Π»ΠΈΡΠ½ΠΈΡ ΠΎΠ·ΠΎΠ½Π° Π½Π° ΠΌΠΎΡΡΠΎΡΡΠ½ΠΊΡΠΈΠΎΠ½Π°Π»ΡΠ½ΡΠ΅ ΠΎΡΠΎΠ±Π΅Π½Π½ΠΎΡΡΠΈ ΠΌΡΠ³ΠΊΠΈΡ
ΡΠΊΠ°Π½Π΅ΠΉ ΡΠΎΡΠΎΠ²ΠΎΠΉ ΠΏΠΎΠ»ΠΎΡΡΠΈ ΠΏΡΠΈ ΠΌΠΎΠ΄Π΅Π»ΠΈΡΠΎΠ²Π°Π½ΠΈΠΈ Ρ
ΡΠΎΠ½ΠΈΡΠ΅ΡΠΊΠΎΠ³ΠΎ ΡΠ΅ΡΠΈΠ΄ΠΈΠ²ΠΈΡΡΡΡΠ΅Π³ΠΎ Π°ΡΡΠΎΠ·Π½ΠΎΠ³ΠΎ ΡΡΠΎΠΌΠ°ΡΠΈΡΠ°. ΠΡΠΎΠ²Π΅Π΄Π΅Π½ΠΎ ΡΠΊΡΠΏΠ΅ΡΠΈΠΌΠ΅Π½ΡΠ°Π»ΡΠ½ΠΎΠ΅ ΠΈΡΡΠ»Π΅Π΄ΠΎΠ²Π°Π½ΠΈΠ΅ Π΄Π»Ρ ΠΈΠ·ΡΡΠ΅Π½ΠΈΡ ΠΌΠΎΡΡΠΎΡΡΠ½ΠΊΡΠΈΠΎΠ½Π°Π»ΡΠ½ΠΎΠ³ΠΎ ΡΠΎΡΡΠΎΡΠ½ΠΈΡ ΡΠΊΠ°Π½Π΅ΠΉ ΡΠ»ΠΈΠ·ΠΈΡΡΠΎΠΉ ΠΎΠ±ΠΎΠ»ΠΎΡΠΊΠΈ ΠΏΠΎΠ»ΠΎΡΡΠΈ ΡΡΠ° ΠΏΡΠΈ Π₯Π ΠΠ‘ Π½Π° ΠΎΡΠ½ΠΎΠ²Π΅ ΡΠ°Π½Π΅Π΅ ΠΏΡΠ΅Π΄Π»ΠΎΠΆΠ΅Π½Π½ΠΎΠΉ ΠΈ ΡΠΈΡΠΎΠΊΠΎ ΠΏΡΠΈΠΌΠ΅Π½ΡΠ΅ΠΌΠΎΠΉ ΠΌΠΎΠ΄Π΅Π»ΠΈ Ρ ΠΈΡΠΏΠΎΠ»ΡΠ·ΠΎΠ²Π°Π½ΠΈΠ΅ΠΌ ΠΎΠ²Π°Π»ΡΠ±ΡΠΌΠΈΠ½Π° ΠΈ Π³ΠΈΠ΄ΡΠΎΠΊΡΠΈΠ΄Π° Π°Π»ΡΠΌΠΈΠ½ΠΈΡ. Π‘ΡΠΎΡΠΌΠΈΡΠΎΠ²Π°Π½Ρ Π΄Π²Π΅ Π³ΡΡΠΏΠΏΡ ΠΆΠΈΠ²ΠΎΡΠ½ΡΡ
(Π³ΠΎΠ»Π»Π°Π½Π΄ΡΠΊΠΈΠ΅ ΠΊΡΠΎΠ»ΠΈ, ΡΠ°ΠΌΡΡ, Π²ΠΎΠ·ΡΠ°ΡΡ ΡΡΠΈ ΠΌΠ΅ΡΡΡΠ°, Π²Π΅Ρ 2-2,4 ΠΊΠ³). I Π³ΡΡΠΏΠΏΠ° ΠΈΠ· 8 ΠΆΠΈΠ²ΠΎΡΠ½ΡΡ
Ρ ΠΈΠ·ΠΌΠ΅Π½Π΅Π½ΠΈΡΠΌΠΈ ΡΠ»ΠΈΠ·ΠΈΡΡΠΎΠΉ ΠΎΠ±ΠΎΠ»ΠΎΡΠΊΠΈ ΡΠΎΡΡΠ°Π²ΠΈΠ»Π° Π³ΡΡΠΏΠΏΡ ΡΡΠ°Π²Π½Π΅Π½ΠΈΡ. II Π³ΡΡΠΏΠΏΠ° ΠΈΠ· 8 ΠΆΠΈΠ²ΠΎΡΠ½ΡΡ
Ρ ΠΈΠ·ΠΌΠ΅Π½Π΅Π½ΠΈΡΠΌΠΈ ΡΠ»ΠΈΠ·ΠΈΡΡΠΎΠΉ ΠΎΠ±ΠΎΠ»ΠΎΡΠΊΠΈ ΡΠΎΡΠΎΠ²ΠΎΠΉ ΠΏΠΎΠ»ΠΎΡΡΠΈ ΠΏΠΎΠ»ΡΡΠ°Π»Π° ΠΎΠ·ΠΎΠ½ΠΎΡΠ΅ΡΠ°ΠΏΠΈΡ. ΠΡΠΎΠ²Π΅Π΄Π΅Π½ΠΎ Π³ΠΈΡΡΠΎΠ»ΠΎΠ³ΠΈΡΠ΅ΡΠΊΠΎΠ΅ ΠΈΡΡΠ»Π΅Π΄ΠΎΠ²Π°Π½ΠΈΠ΅.
ΠΠΈΠΊΡΠΎΡΠΊΠΎΠΏΠΈΡΠ΅ΡΠΊΠΎΠ΅ ΠΈΡΡΠ»Π΅Π΄ΠΎΠ²Π°Π½ΠΈΠ΅ ΡΠΊΠ°Π½Π΅ΠΉ ΠΏΠΎΠΊΠ°Π·Π°Π»ΠΎ, ΡΡΠΎ ΠΎΠ·ΠΎΠ½ΠΎΡΠ΅ΡΠ°ΠΏΠΈΡ ΡΠΌΠ΅Π½ΡΡΠ°Π΅Ρ ΠΏΡΠΈΠ·Π½Π°ΠΊΠΈ Π²ΠΎΡΠΏΠ°Π»Π΅Π½ΠΈΡ, ΠΎΡΠ΅ΠΊΠ° ΠΈ ΡΠΏΠΎΡΠΎΠ±ΡΡΠ²ΡΠ΅Ρ Π·Π°ΠΆΠΈΠ²Π»Π΅Π½ΠΈΡ ΡΠ·Π²Π΅Π½Π½ΡΡ
Π΄Π΅ΡΠ΅ΠΊΡΠΎΠ²: Π½Π°Π±Π»ΡΠ΄Π°Π΅ΡΡΡ ΠΊΠ°ΠΊ ΠΈΡΡΠ΅Π·Π½ΠΎΠ²Π΅Π½ΠΈΠ΅ Π½Π΅ΠΊΡΠΎΠ±ΠΈΠΎΡΠΈΡΠ΅ΡΠΊΠΈΡ
ΠΏΡΠΎΡΠ΅ΡΡΠΎΠ², ΡΠΏΠΈΡΠ΅Π»ΠΈΠ·Π°ΡΠΈΡ Π°ΡΡΠΎΠ·Π½ΡΡ
ΠΏΠΎΡΠ°ΠΆΠ΅Π½ΠΈΠΉ, Π°ΠΊΠ°Π½ΡΠΎΠ·, Π²ΡΡΠ°ΠΆΠ΅Π½Π½ΠΎΠ΅ ΡΠΌΠ΅Π½ΡΡΠ΅Π½ΠΈΠ΅ Π²ΠΎΡΠΏΠ°Π»ΠΈΡΠ΅Π»ΡΠ½ΡΡ
ΠΊΠ»Π΅ΡΠΎΠΊ ΠΈ ΠΈΠ·ΠΌΠ΅Π½Π΅Π½ΠΈΠ΅ ΠΊΠ»Π΅ΡΠΎΡΠ½ΠΎΠ³ΠΎ ΠΎΡΠ½ΠΎΡΠ΅Π½ΠΈΡ - Π½Π΅ΠΉΡΡΠΎΡΠΈΠ»Ρ Ρ 38,30Β±2,46% Π΄ΠΎ 6,34Β±0,63%, ΡΠΎΠ·ΠΈΠ½ΠΎΡΠΈΠ»Ρ - Ρ 5,49Β±0,23% Π΄ΠΎ 2,87Β±0,05%, Π²ΠΎΡΡΡΠ°Π½ΠΎΠ²Π»Π΅Π½ΠΈΠ΅ ΠΊΠ»Π΅ΡΠΎΡΠ½ΡΡ
ΡΠ»ΠΎΠ΅Π² ΡΠΏΠΈΡΠ΅Π»ΠΈΡ, ΡΠΌΠ΅ΡΠ΅Π½Π½ΠΎ Π²ΡΡΠ°ΠΆΠ΅Π½Π½ΡΠΉ ΡΠΊΠ»Π΅ΡΠΎΠ· ΡΠΎΡΠΎΡΠΊΠΎΠ²ΠΎΠ³ΠΎ ΡΠ»ΠΎΡ ΡΠΎΠ±ΡΡΠ²Π΅Π½Π½ΠΎΠΉ ΠΏΠ»Π°ΡΡΠΈΠ½ΠΊΠΈ. ΠΠΎΠ»ΡΡΠ΅Π½Π½ΡΠ΅ ΡΠ΅Π·ΡΠ»ΡΡΠ°ΡΡ ΠΏΠΎΠ·Π²ΠΎΠ»ΡΡΡ Π·Π°ΠΊΠ»ΡΡΠΈΡΡ, ΡΡΠΎ ΠΎΠ·ΠΎΠ½ΠΎΡΠ΅ΡΠ°ΠΏΠΈΡ ΡΠΏΠΎΡΠΎΠ±ΡΡΠ²ΡΠ΅Ρ ΠΊΠΎΡΡΠ΅ΠΊΡΠΈΠΈ ΡΠΊΠ°Π½Π΅Π²ΡΡ
ΠΈΠ·ΠΌΠ΅Π½Π΅Π½ΠΈΠΉ ΠΏΡΠΈ Ρ
ΡΠΎΠ½ΠΈΡΠ΅ΡΠΊΠΎΠΌ ΡΠ΅ΡΠΈΠ΄ΠΈΠ²ΠΈΡΡΡΡΠ΅ΠΌ Π°ΡΡΠΎΠ·Π½ΠΎΠΌ ΡΡΠΎΠΌΠ°ΡΠΈΡΠ΅
On the Nature of Unconfirmed Supernovae
We study the nature of 39 unconfirmed supernovae (SNe) from the sky area
covered by the Sloan Digital Sky Survey (SDSS) Data Release 8 (DR8), using
available photometric and imaging data and intensive literature search. We
confirm that 21 objects are real SNe, 2 are Galactic stars, 4 are probable SNe,
and 12 remain unconfirmed events. The probable types for 4 objects are
suggested: 3 SNe are of probable type Ia, and SN 1953H is probable type II SN.
In addition, we identify the host galaxy of SN 1976N and correct the
offsets/coordinates of SNe 1958E, 1972F, and 1976N.Comment: 9 pages, 4 figures, 5 tables, published in Astrophysics (English
translation of Astrofizika
Supernovae in paired galaxies
We investigate the influence of close neighbor galaxies on the properties of
supernovae (SNe) and their host galaxies using 56 SNe located in pairs of
galaxies with different levels of star formation (SF) and nuclear activity. The
mean distance of type II SNe from nuclei of hosts is greater by about a factor
of 2 than that of type Ibc SNe. The distributions and mean distances of SNe are
consistent with previous results compiled with the larger sample. For the first
time it is shown that SNe Ibc are located in pairs with significantly smaller
difference of radial velocities between components than pairs containing SNe Ia
and II. We consider this as a result of higher star formation rate (SFR) of
these closer systems of galaxies.Comment: 2 pages. arXiv admin note: text overlap with arXiv:1312.494
Paired galaxies with different activity levels and their supernovae
We investigate the influence of close neighbor galaxies on the properties of
supernovae (SNe) and their host galaxies using 56 SNe located in pairs of
galaxies with different levels of star formation (SF) and nuclear activity. The
statistical study of SN hosts shows that there is no significant difference
between morphologies of hosts in our sample and the larger general sample of SN
hosts in the Sloan Digital Sky Survey (SDSS) Data Release 8 (DR8). The mean
distance of type II SNe from nuclei of hosts is greater by about a factor of 2
than that of type Ibc SNe. The distributions and mean distances of SNe are
consistent with previous results compiled with the larger sample. For the first
time it is shown that SNe Ibc are located in pairs with significantly smaller
difference of radial velocities between components than pairs containing SNe Ia
and II. We consider this as a result of higher star formation rate (SFR) of
these closer systems of galaxies. SN types are not correlated with the
luminosity ratio of host and neighbor galaxies in pairs. The orientation of SNe
with respect to the preferred direction toward neighbor galaxy is found to be
isotropic and independent of kinematical properties of the galaxy pair.Comment: 10 pages, 2 figures, 5 tables, online data, published in Astrophysics
and Space Scienc
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Room temperature "optical nanodiamond hyperpolarizer": Physics, design, and operation.
Dynamic Nuclear Polarization (DNP) is a powerful suite of techniques that deliver multifold signal enhancements in nuclear magnetic resonance (NMR) and MRI. The generated athermal spin states can also be exploited for quantum sensing and as probes for many-body physics. Typical DNP methods require the use of cryogens, large magnetic fields, and high power microwave excitation, which are expensive and unwieldy. Nanodiamond particles, rich in Nitrogen-Vacancy (NV) centers, have attracted attention as alternative DNP agents because they can potentially be optically hyperpolarized at room temperature. Here, unraveling new physics underlying an optical DNP mechanism first introduced by Ajoy et al. [Sci. Adv. 4, eaar5492 (2018)], we report the realization of a miniature "optical nanodiamond hyperpolarizer," where 13C nuclei within the diamond particles are hyperpolarized via the NV centers. The device occupies a compact footprint and operates at room temperature. Instrumental requirements are very modest: low polarizing fields, low optical and microwave irradiation powers, and convenient frequency ranges that enable miniaturization. We obtain the best reported optical 13C hyperpolarization in diamond particles exceeding 720 times of the thermal 7 T value (0.86% bulk polarization), corresponding to a ten-million-fold gain in averaging time to detect them by NMR. In addition, the hyperpolarization signal can be background-suppressed by over two-orders of magnitude, retained for multiple-minute long periods at low fields, and deployed efficiently even to 13C enriched particles. Besides applications in quantum sensing and bright-contrast MRI imaging, this work opens possibilities for low-cost room-temperature DNP platforms that relay the 13C polarization to liquids in contact with the high surface-area particles
Enhanced dynamic nuclear polarization via swept microwave frequency combs
Dynamic Nuclear Polarization (DNP) has enabled enormous gains in magnetic
resonance signals and led to vastly accelerated NMR/MRI imaging and
spectroscopy. Unlike conventional cw-techniques, DNP methods that exploit the
full electron spectrum are appealing since they allow direct participation of
all electrons in the hyperpolarization process. Such methods typically entail
sweeps of microwave radiation over the broad electron linewidth to excite DNP,
but are often inefficient because the sweeps, constrained by adiabaticity
requirements, are slow. In this paper we develop a technique to overcome the
DNP bottlenecks set by the slow sweeps, employing a swept microwave frequency
comb that increases the effective number of polarization transfer events while
respecting adiabaticity constraints. This allows a multiplicative gain in DNP
enhancement, scaling with the number of comb frequencies and limited only by
the hyperfine-mediated electron linewidth. We demonstrate the technique for the
optical hyperpolarization of 13C nuclei in powdered microdiamonds at low
fields, increasing the DNP enhancement from 30 to 100 measured with respect to
the thermal signal at 7T. For low concentrations of broad linewidth electron
radicals, e.g. TEMPO, these multiplicative gains could exceed an order of
magnitude.Comment: Contains supplementary inf
Supernovae and their host galaxies - IV. The distribution of supernovae relative to spiral arms
Using a sample of 215 supernovae (SNe), we analyze their positions relative
to the spiral arms of their host galaxies, distinguishing grand-design (GD)
spirals from non-GD (NGD) galaxies. We find that: (1) in GD galaxies, an offset
exists between the positions of Ia and core-collapse (CC) SNe relative to the
peaks of arms, while in NGD galaxies the positions show no such shifts; (2) in
GD galaxies, the positions of CC SNe relative to the peaks of arms are
correlated with the radial distance from the galaxy nucleus. Inside (outside)
the corotation radius, CC SNe are found closer to the inner (outer) edge. No
such correlation is observed for SNe in NGD galaxies nor for SNe Ia in either
galaxy class; (3) in GD galaxies, SNe Ibc occur closer to the leading edges of
the arms than do SNe II, while in NGD galaxies they are more concentrated
towards the peaks of arms. In both samples of hosts, the distributions of SNe
Ia relative to the arms have broader wings. These observations suggest that
shocks in spiral arms of GD galaxies trigger star formation in the leading
edges of arms affecting the distributions of CC SNe (known to have short-lived
progenitors). The closer locations of SNe Ibc vs. SNe II relative to the
leading edges of the arms supports the belief that SNe Ibc have more massive
progenitors. SNe Ia having less massive and older progenitors, have more time
to drift away from the leading edge of the spiral arms.Comment: 19 pages, 10 figures, 11 tables, resubmitted to MNRAS after
addressing referee's comment
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