22 research outputs found
Photo-isolation chemistry for high-resolution and deep spatial transcriptome with mouse tissue sections
Photo-isolation chemistry (PIC) enables isolation of transcriptome information from locally defined areas by photo-irradiation. Here, we present an optimized PIC protocol for formalin-fixed frozen and paraffin mouse sections and fresh-frozen mouse sections. We describe tissue section preparation and permeabilization, followed by in situ reverse transcription using photo-caged primers. We then detail immunostaining and UV-mediated uncaging to the target areas, followed by linear amplification of uncaged cDNAs, library preparation, and quantification. This protocol can be applied to various animal tissue types
High-depth spatial transcriptome analysis by photo-isolation chemistry
光照射を用いた超高解像度な遺伝子解析技術の開発に成功 --組織内に潜むがん細胞の病理診断などに応用可能--. 京都大学プレスリリース. 2021-07-27.In multicellular organisms, expression profiling in spatially defined regions is crucial to elucidate cell interactions and functions. Here, we establish a transcriptome profiling method coupled with photo-isolation chemistry (PIC) that allows the determination of expression profiles specifically from photo-irradiated regions of interest. PIC uses photo-caged oligodeoxynucleotides for in situ reverse transcription. PIC transcriptome analysis detects genes specifically expressed in small distinct areas of the mouse embryo. Photo-irradiation of single cells demonstrated that approximately 8, 000 genes were detected with 7 × 10⁴ unique read counts. Furthermore, PIC transcriptome analysis is applicable to the subcellular and subnuclear microstructures (stress granules and nuclear speckles, respectively), where hundreds of genes can be detected as being specifically localised. The spatial density of the read counts is higher than 100 per square micrometre. Thus, PIC enables high-depth transcriptome profiles to be determined from limited regions up to subcellular and subnuclear resolutions
Discovery of a new dwarf nova, TSS J022216.4+412259.9: WZ Sge-type dwarf novae breaking the shortest superhump period record
We report on the time-resolved CCD photometry of a newly discovered variable
star, TSS J022216.4+412259.9 during the outburst in 2005 November-December
brightening. The obtained light curves unambiguously showed 0.2-0.3 mag
modulations, which we confirmed to be the superhump observed among SU UMa-type
dwarf novae. We also performed a period search for the data obtained during the
outburst plateau phase, and revealed the existence of the two periodicities:
0.054868(98) days for the first two nights and 0.055544(26) days for the
following plateau phase. This bi-periodicity is hardly observed in usual SU
UMa-type dwarf novae, but characteristic of WZ Sge-type stars. We undoubtedly
detected a rebrightening in the post-outburst stage, which is typical of
short-period SU UMa-type dwarf novae including WZ Sge-type stars. These
observations suggests that TSS J022216.4+412259.9 may be a new WZ Sge stars
breaking the shortest superhump period of 0.05648 days for V592 Her among this
class with a known superhump period so far.Comment: 5 pages, 6 figures, accepted for PASJ lette
Long-term monitoring of the short period SU UMa-type dwarf nova, V844 Herculis
We report on time-resolved CCD photometry of four outbursts of a short-period
SU UMa-type dwarf nova, V844 Herculis. We successfully determined the mean
superhump periods to be 0.05584(64) days, and 0.055883(3) for the 2002 May
superoutburst, and the 2006 April-May superoutburst, respectively. During the
2002 October observations, we confirmed that the outburst is a normal outburst,
which is the first recorded normal outburst in V844 Her. We also examined
superhump period changes during 2002 May and 2006 April-May superoutbursts,
both of which showed increasing superhump period over the course of the plateau
stage. In order to examine the long-term behavior of V844 Her, we analyzed
archival data over the past ten years since the discovery of this binary.
Although photometry is not satisfactory in some superoutbursts, we found that
V844 Her showed no precursors and rebrightenings. Based on the long-term light
curve, we further confirmed V844 Her has shown almost no normal outbursts
despite the fact that the supercycle of the system is estimated to be about 300
days. In order to explain the long-term light curves of V844 Her, evaporation
in the accretion disk may play a role in the avoidance of several normal
outbursts, which does not contradict with the relatively large X-ray luminosity
of V844 Her.Comment: 10 pages, 11 figures, accepted for PAS
Dwarf Novae in the Shortest Orbital Period Regime: I. A New Short Period Dwarf Nova, OT J055717+683226
We report the observation of a new dwarf nova, OT J055717+683226, during its
first-ever recorded superoutburst in December 2006. Our observation shows that
this object is an SU UMa-type dwarf nova having a very short superhump period
of 76.67+/- 0.03 min (0.05324+/-0.00002 d). The next superoutburst was observed
in March 2008. The recurrence time of superoutbursts (supercycle) is, hence,
estimated to be ~480 d. The supercycle is much shorter than those of WZ
Sge-type dwarf novae having supercycles of >~ 10 yr, which are a major
population of dwarf novae in the shortest orbital period regime (<~85 min).
Using a hierarchical cluster analysis, we identified seven groups of dwarf
novae in the shortest orbital period regime. We identified a small group of
objects that have short supercycles, small outburst amplitudes, and large
superhump period excesses, compared with those of WZ Sge stars. OT
J055717+683226 probably belongs to this group.Comment: 14 pages, 11 figures, accepted for publication in PAS
The 2006 November outburst of EG Aquarii: the SU UMa nature revealed
We report time-resolved CCD photometry of the cataclysmic variable EG Aquarii
during the 2006 November outburst During the outburst, superhumps were
unambiguously detected with a mean period of 0.078828(6) days, firstly
classifying the object as an SU UMa-type dwarf nova. It also turned out that
the outburst contained a precursor. At the end of the precursor, immature
profiles of humps were observed. By a phase analysis of these humps, we
interpreted the features as superhumps. This is the second example that the
superhumps were shown during a precursor. Near the maximum stage of the
outburst, we discovered an abrupt shift of the superhump period by
0.002 days. After the supermaximum, the superhump period decreased at the rate
of =, which is typical for SU UMa-type dwarf
novae. Although the outburst light curve was characteristic of SU UMa-type
dwarf novae, long-term monitoring of the variable shows no outbursts over the
past decade. We note on the basic properties of long period and inactive SU
UMa-type dwarf novae.Comment: 9 pages, 7 figures, accepted for PAS
Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae
We systematically surveyed period variations of superhumps in SU UMa-type
dwarf novae based on newly obtained data and past publications. In many
systems, the evolution of superhump period are found to be composed of three
distinct stages: early evolutionary stage with a longer superhump period,
middle stage with systematically varying periods, final stage with a shorter,
stable superhump period. During the middle stage, many systems with superhump
periods less than 0.08 d show positive period derivatives. Contrary to the
earlier claim, we found no clear evidence for variation of period derivatives
between superoutburst of the same object. We present an interpretation that the
lengthening of the superhump period is a result of outward propagation of the
eccentricity wave and is limited by the radius near the tidal truncation. We
interpret that late stage superhumps are rejuvenized excitation of 3:1
resonance when the superhumps in the outer disk is effectively quenched. Many
of WZ Sge-type dwarf novae showed long-enduring superhumps during the
post-superoutburst stage having periods longer than those during the main
superoutburst. The period derivatives in WZ Sge-type dwarf novae are found to
be strongly correlated with the fractional superhump excess, or consequently,
mass ratio. WZ Sge-type dwarf novae with a long-lasting rebrightening or with
multiple rebrightenings tend to have smaller period derivatives and are
excellent candidate for the systems around or after the period minimum of
evolution of cataclysmic variables (abridged).Comment: 239 pages, 225 figures, PASJ accepte
地域活動への住民参加を促すための保健師の支援方法
A地区の地域活動への住民の参加状況と参加条件を明らかにするため、4団体108名を対象に質問紙調査を行った。地域活動への参加条件として重要なのは、健康であること、家族の理解と協力があること、身近な人と一緒に参加できること、活動場所が自宅に近いこと、活動する時間的余裕があること等が明らかとなった。地域活動支援のあり方としては、個人や家族の健康を保持・増進し、地域の人々のつながりを強め、時間・場所・移動手段を工夫し住民が集いやすくすることにより、参加条件を満たすことが有効と考えられた。保健師は、個人や集団が地域活動を活発にするための工夫や連携を図り、個人・集団の力を引き出せるような支援をしていくことが重要であると考えられた