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1 <?xml version="1.0" encoding="UTF-8"?>
2 <rss version="2.0" xmlns:prism="http://purl.org/rss/1.0/modules/prism/">
3 <channel>
4 <title>Publications of the Astronomical Society of Japan Current Issue</title>
5 <link>http://academic.oup.com/pasj</link>
6 <description>
7 </description>
8 <language>en-us</language>
9 <pubDate>Fri, 27 Jan 2023 00:00:00 GMT</pubDate>
10 <lastBuildDate>Mon, 06 Feb 2023 11:48:32 GMT</lastBuildDate>
11 <generator>Silverchair</generator>
12 <item>
13 <title>Distance determination of molecular clouds in the first quadrant of the Galactic plane using deep learning: I. Method and results</title>
14 <link>https://academic.oup.com/pasj/article/75/1/279/6988000?rss=1</link>
15 <pubDate>Fri, 27 Jan 2023 00:00:00 GMT</pubDate>
16 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>Machine learning has been successfully applied in various field but whether it is a viable tool for determining the distance to molecular clouds in the Galaxy is an open question. In the Galaxy, the kinematic distance is commonly employed to represent the distance to a molecular cloud. However, for the inner Galaxy, two different solutions, i.e., the “Near” solution and the “Far” solution, can be derived simultaneously. We attempt to construct a two-class (“Near” or “Far”) inference model using a convolutional neural network (CNN), which is a form of deep learning that can capture spatial features generally. In this study, we use the CO dataset in the first quadrant of the Galactic plane obtained with the Nobeyama 45 m radio telescope (<span style="font-style:italic;">l</span> = 62°–10°, |<span style="font-style:italic;">b</span>| &lt; 1°). In the model, we apply the three-dimensional distribution (position–position–velocity) of the <sup>12</sup>CO (<span style="font-style:italic;">J</span> = 1–0) emissions as the main input. To train the model, a dataset with “Near” or “Far” annotation was created from the H <span style="text-transform:lowercase;font-variant:small-caps;">ii</span> region catalog of the infrared astronomy satellite WISE. Consequently, we construct a CNN model with a $76\% $ accuracy rate on the training dataset. Using the proposed model, we determine the distance to the molecular clouds identified by the CLUMPFIND algorithm. We found that the mass of molecular clouds with a distance of &lt;8.15 kpc identified in the <sup>12</sup>CO data follows a power-law distribution with an index of approximately −2.3 in the mass range <span style="font-style:italic;">M</span> &gt; 10<sup>3</sup> <span style="font-style:italic;">M</span><sub>⊙</sub>. In addition, the detailed molecular gas distribution of the Galaxy, as seen from the Galactic North pole, was determined.</span></description>
17 <prism:volume xmlns:prism="prism">75</prism:volume>
18 <prism:number xmlns:prism="prism">1</prism:number>
19 <prism:startingPage xmlns:prism="prism">279</prism:startingPage>
20 <prism:endingPage xmlns:prism="prism">295</prism:endingPage>
21 <prism:doi xmlns:prism="prism">10.1093/pasj/psac104</prism:doi>
22 <guid>http://doi.org/10.1093/pasj/psac104</guid>
23 </item>
24 <item>
25 <title>Two saturated states of the vertical shear instability in protoplanetary disks with vertically varying cooling times</title>
26 <link>https://academic.oup.com/pasj/article/75/1/233/6986070?rss=1</link>
27 <pubDate>Thu, 12 Jan 2023 00:00:00 GMT</pubDate>
28 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>Turbulence in protoplanetary disks plays an important role in dust evolution and planetesimal formation. The vertical shear instability (VSI) is one of the candidate hydrodynamic mechanisms that can generate turbulence in the outer disk regions. The VSI requires rapid gas cooling in addition to vertical shear. A linear stability analysis suggests that the VSI may not operate around the midplane where gas cooling is inefficient. In this study, we investigate the nonlinear outcome of the VSI in disks with a linearly VSI-stable midplane region. We perform two-dimensional global hydrodynamical simulations of an axisymmetric disk with vertically varying cooling times. The vertical cooling time profile determines the thicknesses of the linearly VSI-stable midplane layer and unstable layers above and below the midplane. We find that the thickness of the midplane stable layer determines the vertical structure of VSI-driven turbulence in the nonlinear saturated state. We identify two types of final saturated state: (i) T states, characterized by vertical turbulent motion penetrating into the VSI-stable midplane layer, and (ii) pT states, characterized by turbulent motion confined in the unstable layers. The pT states are realized when the midplane VSI-stable layer is thicker than two gas scale heights. We also find that the VSI-driven turbulence is largely suppressed at all heights when the VSI-unstable region lying above and below the midplane is thinner than two gas scale heights. We present empirical formulas that predict the strength of VSI-driven turbulence as a function of the thicknesses of the unstable and stable layers. These formulas will be useful for studying how VSI-driven turbulence and dust grains controlling the disk cooling efficiency evolve simultaneously.</span></description>
29 <prism:volume xmlns:prism="prism">75</prism:volume>
30 <prism:number xmlns:prism="prism">1</prism:number>
31 <prism:startingPage xmlns:prism="prism">233</prism:startingPage>
32 <prism:endingPage xmlns:prism="prism">249</prism:endingPage>
33 <prism:doi xmlns:prism="prism">10.1093/pasj/psac107</prism:doi>
34 <guid>http://doi.org/10.1093/pasj/psac107</guid>
35 </item>
36 <item>
37 <title>BVRI polarization of stars in the direction of Stock 19</title>
38 <link>https://academic.oup.com/pasj/article/75/1/269/6984983?rss=1</link>
39 <pubDate>Wed, 11 Jan 2023 00:00:00 GMT</pubDate>
40 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>We present <span style="font-style:italic;">BVRI</span> polarimetric measurements of nine bright stars in a 15′-square region centered on Stock 19. Seven of them satisfy the Serkowski equation for star light polarization due to interstellar dust. This allowed us to estimate the degree of maximum polarization (<span style="font-style:italic;">p</span><sub>max</sub>) and the wavelength of maximum polarization (λ<sub>max</sub>). Along this line of sight, <span style="font-style:italic;">p</span><sub>max</sub> ranges from 0.332% to 0.948%, and the average λ<sub>max</sub> of 0.542 ± 0.018 μm yields a total-to-selective extinction ratio <span style="font-style:italic;">RV</span> = 3.04 ± 0.11. Four of the observed stars were previously listed as high-probability members of Stock 19. However, based on their Gaia distances, they are spread out along the line of sight and show a correlation between polarization and distance that is typical for the diffuse interstellar medium. The extinction, as obtained from dust maps, and the Planck 353 GHz polarization are low for this line of sight, additionally suggesting that these stars might not represent an actual cluster. The polarization parameters of three of the observed stars indicate the possible presence of an intrinsic polarization component, likely due to circumstellar material.</span></description>
41 <prism:volume xmlns:prism="prism">75</prism:volume>
42 <prism:number xmlns:prism="prism">1</prism:number>
43 <prism:startingPage xmlns:prism="prism">269</prism:startingPage>
44 <prism:endingPage xmlns:prism="prism">278</prism:endingPage>
45 <prism:doi xmlns:prism="prism">10.1093/pasj/psac108</prism:doi>
46 <guid>http://doi.org/10.1093/pasj/psac108</guid>
47 </item>
48 <item>
49 <title>Detection of a bright burst from the repeating fast radio burst 20201124A at 2 GHz</title>
50 <link>https://academic.oup.com/pasj/article/75/1/199/6983077?rss=1</link>
51 <pubDate>Wed, 11 Jan 2023 00:00:00 GMT</pubDate>
52 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>We present a detection of a bright burst from the fast radio burst (FRB) 20201124A, which is one of the most active repeating FRBs, based on <span style="font-style:italic;">S</span>-band observations with the 64 m radio telescope at the Usuda Deep Space Center/JAXA. This is the first FRB observed by using a Japanese facility. Our detection at 2 GHz in 2022 February is the highest frequency for this FRB and the fluence of &gt;189 Jy ms is one of the brightest bursts from this FRB source. We place an upper limit on the spectral index α = −2.14 from the detection of the <span style="font-style:italic;">S</span> band and non-detection of the <span style="font-style:italic;">X</span> band at the same time. We compare the event rate of the detected burst with those from previous research and suggest that the power law of the luminosity function might be broken at lower fluence and the fluences of bright FRBs are distributed up to over 2 GHz with the power law against frequency. In addition, we show that the energy density of the burst detected in this work is comparable to the bright population of one-off FRBs. We propose that repeating FRBs can be as bright as one-off FRBs and only their brightest bursts might be detected, so some repeating FRBs intrinsically might have been classified as one-off FRBs.</span></description>
53 <prism:volume xmlns:prism="prism">75</prism:volume>
54 <prism:number xmlns:prism="prism">1</prism:number>
55 <prism:startingPage xmlns:prism="prism">199</prism:startingPage>
56 <prism:endingPage xmlns:prism="prism">207</prism:endingPage>
57 <prism:doi xmlns:prism="prism">10.1093/pasj/psac101</prism:doi>
58 <guid>http://doi.org/10.1093/pasj/psac101</guid>
59 </item>
60 <item>
61 <title>Twisted magnetic field in star formation processes of L1521 F revealed by submillimeter dual-band polarimetry using the James Clerk Maxwell Telescope</title>
62 <link>https://academic.oup.com/pasj/article/75/1/120/6979699?rss=1</link>
63 <pubDate>Mon, 09 Jan 2023 00:00:00 GMT</pubDate>
64 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>Understanding the initial conditions of star formation requires both observational studies and theoretical works taking into account the magnetic field, which plays an important role in star formation processes. Herein, we study the young nearby dense cloud core L1521 F [<span style="font-style:italic;">n</span>(H<sub>2</sub>) ∼10<sup>4−6</sup> cm<sup>−3</sup>] in the Taurus Molecular Cloud. This dense core hosts a 0.2 <span style="font-style:italic;">M</span><sub>⊙</sub> protostar, categorized as a very low luminosity object with complex velocity structures, particularly in the vicinity of the protostar. To trace the magnetic field within the dense core, we conducted high-sensitivity submillimeter polarimetry of the dust continuum at λ = 850 μm and 450 μm using the POL-2 polarimeter situated in front of the SCUBA-2 submillimeter bolometer camera on the James Clerk Maxwell Telescope. This was compared with millimeter polarimetry taken at λ = 3.3 mm with ALMA. The magnetic field was detected at λ = 850 μm in the peripheral region, which is threaded in a north–south direction, while the central region traced at λ = 450 μm shows a magnetic field with an east–west direction, i.e., orthogonal to that of the peripheral region. Magnetic field strengths are estimated to be ∼70 μG and 200 μG in the peripheral and central regions, respectively, using the Davis–Chandrasekhar–Fermi method. The resulting mass-to-flux ratio of three times larger than that of magnetically critical state for both regions indicates that L 1521 F is magnetically supercritical, i.e., gravitational forces dominate over magnetic turbulence forces. Combining observational data with magnetohydrodynamic simulations, detailed parameters of the morphological properties of this puzzling object are derived for the first time.</span></description>
65 <prism:volume xmlns:prism="prism">75</prism:volume>
66 <prism:number xmlns:prism="prism">1</prism:number>
67 <prism:startingPage xmlns:prism="prism">120</prism:startingPage>
68 <prism:endingPage xmlns:prism="prism">127</prism:endingPage>
69 <prism:doi xmlns:prism="prism">10.1093/pasj/psac094</prism:doi>
70 <guid>http://doi.org/10.1093/pasj/psac094</guid>
71 </item>
72 <item>
73 <title>The light curve simulations of the 2021 anomalous event in SS Cygni</title>
74 <link>https://academic.oup.com/pasj/article/75/1/250/6966542?rss=1</link>
75 <pubDate>Sat, 31 Dec 2022 00:00:00 GMT</pubDate>
76 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>The prototype dwarf nova SS Cyg unexpectedly exhibited an anomalous event in its light curve in the early few months of 2021 in which regular dwarf nova-type outbursts stopped, and only small-amplitude fluctuations occurred. Inspired by this event, we have performed numerical simulations of light curves of SS Cyg by varying mass transfer rates and varying viscosity parameters in the cool disk. We have also studied the effect of gas-stream overflows beyond the outer disk edge in the light curve simulations. We have confirmed that the enhanced mass transfer is not likely to be responsible for the 2021 anomalous event or its forerunner. We have found that the enhancement of the viscosity in the disk may reproduce the forerunner of that event but may not be sufficient to explain the 2021 anomalous event, although the latter result might be particular to the thermal equilibrium curve we used. Within our simulations, a model of the gas-stream overflow with a slightly higher mass transfer rate than that of our standard model reproduces light curves similar to the 2021 anomalous event. We suggest that the gas-stream overflow is necessary to reproduce that event. The gas-stream overflow may also be responsible for the abnormally high X-ray flux during the normal quiescent state in SS Cyg.</span></description>
77 <prism:volume xmlns:prism="prism">75</prism:volume>
78 <prism:number xmlns:prism="prism">1</prism:number>
79 <prism:startingPage xmlns:prism="prism">250</prism:startingPage>
80 <prism:endingPage xmlns:prism="prism">268</prism:endingPage>
81 <prism:doi xmlns:prism="prism">10.1093/pasj/psac106</prism:doi>
82 <guid>http://doi.org/10.1093/pasj/psac106</guid>
83 </item>
84 <item>
85 <title>An expanding ring of the hypercompact H ii region W 49 N:A2</title>
86 <link>https://academic.oup.com/pasj/article/75/1/225/6964915?rss=1</link>
87 <pubDate>Thu, 29 Dec 2022 00:00:00 GMT</pubDate>
88 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>We present 250 GHz continuum and H29α line data toward W 49 N:A2, a hypercompact H <span style="text-transform:lowercase;font-variant:small-caps;">ii</span> region ionized by an O9 star. The data obtained with ALMA at a resolution of ∼0${_{.}^{\prime\prime}}$05 (600 au) confirmed the presence of an ionized ring with a radius of ∼700 au inclined by ∼50° (0° for pole-on). It has a width of ∼1000 au and is relatively flat with a scale height of less than several hundred au. The tilted ring, or the apparent ellipse, has a prominent velocity difference between its NW and SE ridges along the minor axis, suggesting that it is expanding in the equatorial plane at a velocity of 13.2 km s<sup>−1</sup>. The ring also shows a hint of rotation at 2.7 km s<sup>−1</sup>, which is significantly (2.5 σ) smaller than the Kepler velocity of 5.2 km s<sup>−1</sup> at its radius around the 20 <span style="font-style:italic;">M</span><sub>⊙</sub> star. This can be interpreted as that the ring gas has been transported from the radius of ∼170 au by conserving its original specific angular momentum that it had there. The ionized ring may thus be a remnant of the accretion disk that fed the O9 star, the radiation or magnetic activities of which became so strong that the disk accretion was reversed due to the intense thermal or magneto-hydrodynamic pressure around the star. The data has revealed a rare example of how a massive star terminates its accretion at the end of its formation, transforming a hypercompact H <span style="text-transform:lowercase;font-variant:small-caps;">ii</span> region into an ultracompact H <span style="text-transform:lowercase;font-variant:small-caps;">ii</span> region.</span></description>
89 <prism:volume xmlns:prism="prism">75</prism:volume>
90 <prism:number xmlns:prism="prism">1</prism:number>
91 <prism:startingPage xmlns:prism="prism">225</prism:startingPage>
92 <prism:endingPage xmlns:prism="prism">232</prism:endingPage>
93 <prism:doi xmlns:prism="prism">10.1093/pasj/psac105</prism:doi>
94 <guid>http://doi.org/10.1093/pasj/psac105</guid>
95 </item>
96 <item>
97 <title>Multi-chord observation of stellar occultation by the near-Earth asteroid (3200) Phaethon on 2021 October 3 (UTC) with very high accuracy</title>
98 <link>https://academic.oup.com/pasj/article/75/1/153/6947807?rss=1</link>
99 <pubDate>Tue, 20 Dec 2022 00:00:00 GMT</pubDate>
100 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>We observed a stellar occultation by (3200) Phaethon, which occurred in western Japan on 2021 October 3 (UTC). This observation was requested by the DESTINY<sup>+</sup> mission team, which plans to conduct a flyby of asteroid Phaethon in 2028. Overall, this research effort contributes towards a large-scale observation campaign with a total of 72 observers observing from western Japan to southern Korea. 36 stations were established, and stellar occultation by the asteroid Phaethon was detected in 18 of them. This is the first time that this many multiple chord observations have been made for such a small asteroid (it has a diameter of 5–6 km). Observational reductions show that the apparent cross-section of Phaethon at the time of the occultation could be approximated using an ellipse with a major diameter of 6.12 ± 0.07 km and a minor diameter of 4.14 ± 0.07 km, and a position angle of 117.°4 ± 1.°5. As can be seen from the small error bars of the fitted ellipse, we have succeeded in estimating the shape and size of the asteroid with an extremely high degree of accuracy. Our observation results, together with other observations, will be used to create a 3D model of Phaethon and to improve its orbit. The instruments that we used for this observation are commonly used by many amateur astronomers in Japan for occultation observations and are not difficult to obtain. This paper describes the method and results of our observations using a CMOS camera and a GPS module, so that many people can participate in occultation observations in the future.</span></description>
101 <prism:volume xmlns:prism="prism">75</prism:volume>
102 <prism:number xmlns:prism="prism">1</prism:number>
103 <prism:startingPage xmlns:prism="prism">153</prism:startingPage>
104 <prism:endingPage xmlns:prism="prism">168</prism:endingPage>
105 <prism:doi xmlns:prism="prism">10.1093/pasj/psac096</prism:doi>
106 <guid>http://doi.org/10.1093/pasj/psac096</guid>
107 </item>
108 <item>
109 <title>East Asian VLBI Network astrometry toward the extreme outer Galaxy: Kinematic distance with the proper motion of G034.84−00.95</title>
110 <link>https://academic.oup.com/pasj/article/75/1/208/6916925?rss=1</link>
111 <pubDate>Fri, 16 Dec 2022 00:00:00 GMT</pubDate>
112 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>We aim to reveal the structure and kinematics of the Outer Scutum–Centaurus (OSC) arm located on the far side of the Milky Way through very long baseline interferometry (VLBI) astrometry using KaVA, which is composed of KVN (the Korean VLBI Network) and VERA (VLBI Exploration of Radio Astrometry). We report the proper motion of a 22 GHz H<sub>2</sub>O maser source, which is associated with the star-forming region G034.84−00.95, to be (μ<sub>α</sub>cos δ, μ<sub>δ</sub>) = (−1.61 ± 0.18, −4.29 ± 0.16) mas yr<sup>−1</sup> in equatorial coordinates (J2000.0). We estimate the 2D kinematic distance to the source to be 18.6 ± 1.0 kpc, which is derived from the variance weighted average of kinematic distances with local standard of rest velocity and the galactic-longitude component of the measured proper motion. Our result places the source in the OSC arm and implies that G034.84−00.95 is moving away from the Galactic plane with a vertical velocity of −38 ± 16 km s<sup>−1</sup>. Since the H <span style="text-transform:lowercase;font-variant:small-caps;">i</span> supershell GS033+06−49 is located at a kinematic distance roughly equal to that of G034.84−00.95, it is expected that gas circulation occurs between the outer Galactic disk around G034.84−00.95 with a Galactocentric distance of $12.8^{+1.0}_{-0.9}\:$kpc and the halo. We evaluate possible origins of the fast vertical motion of G034.84−00.95, which are (1) supernova explosions and (2) cloud collisions with the Galactic disk. However, neither of these possibilities are matched with the results of VLBI astrometry or the spatial distributions of H <span style="text-transform:lowercase;font-variant:small-caps;">ii</span> regions and H <span style="text-transform:lowercase;font-variant:small-caps;">i</span> gas.</span></description>
113 <prism:volume xmlns:prism="prism">75</prism:volume>
114 <prism:number xmlns:prism="prism">1</prism:number>
115 <prism:startingPage xmlns:prism="prism">208</prism:startingPage>
116 <prism:endingPage xmlns:prism="prism">224</prism:endingPage>
117 <prism:doi xmlns:prism="prism">10.1093/pasj/psac102</prism:doi>
118 <guid>http://doi.org/10.1093/pasj/psac102</guid>
119 </item>
120 <item>
121 <title>X-ray and optical spectroscopic study of a γ Cassiopeiae analog source π Aquarii</title>
122 <link>https://academic.oup.com/pasj/article/75/1/177/6896272?rss=1</link>
123 <pubDate>Wed, 14 Dec 2022 00:00:00 GMT</pubDate>
124 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>γ Cas analog sources are a subset of Be stars that emit intense and hard X-ray emission. Two competing ideas for their X-ray production mechanism are (a) the magnetic activities of the Be star and its disk and (b) the accretion from the Be star to an unidentified compact object. Among such sources, π Aqr plays a pivotal role as it is one of the only two spectroscopic binaries observed for many orbital cycles and one of the three sources with X-ray brightness sufficient for detailed X-ray spectroscopy. Bjorkman et al. (2002, ApJ, 573, 812) estimated the secondary mass &gt;2.0 <span style="font-style:italic;">M</span><sub>⊙</sub> with optical spectroscopy, which would argue against the compact object being a white dwarf (WD). However, their dynamical mass solution is inconsistent with an evolutionary solution and their radial velocity measurement is inconsistent with later work by Nazé et al. (2019, A&amp;A, 632, A23). We revisit this issue by adding a new data set with the NuSTAR X-ray observatory and the HIDES échelle spectrograph. We found that the radial velocity amplitude is consistent with Nazé et al. (2019, A&amp;A, 632, A23), which is only half of that claimed by Bjorkman et al. (2002, ApJ, 573, 812). Fixing the radial velocity amplitude of the primary, the secondary mass is estimated as &lt;1.4 <span style="font-style:italic;">M</span><sub>⊙</sub> over an assumed range of the primary mass and the inclination angle. We further constrained the inclination angle and the secondary mass independently by fitting the X-ray spectra with a non-magnetic or magnetic accreting WD model under the assumption that the secondary is indeed a WD. The two results match well. We thus argue that the possibility of the secondary being a WD should not be excluded for π Aqr.</span></description>
125 <prism:volume xmlns:prism="prism">75</prism:volume>
126 <prism:number xmlns:prism="prism">1</prism:number>
127 <prism:startingPage xmlns:prism="prism">177</prism:startingPage>
128 <prism:endingPage xmlns:prism="prism">186</prism:endingPage>
129 <prism:doi xmlns:prism="prism">10.1093/pasj/psac099</prism:doi>
130 <guid>http://doi.org/10.1093/pasj/psac099</guid>
131 </item>
132 <item>
133 <title>Modeling of geocoronal solar wind charge exchange events detected with Suzaku</title>
134 <link>https://academic.oup.com/pasj/article/75/1/128/6887604?rss=1</link>
135 <pubDate>Mon, 12 Dec 2022 00:00:00 GMT</pubDate>
136 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>A model of geocoronal solar wind charge exchange (SWCX) emission was built and compared to five Suzaku detections of bright geocoronal SWCX events. An exospheric neutral hydrogen distribution model, charge exchange cross-sections, solar wind ion data taken with the ACE and WIND satellites, and magnetic field models of the Earth’s magnetosphere are all combined in order to predict time-variable geocoronal SWCX emission depending on line-of-sight directions of the Suzaku satellite. The modeled average intensities of O <span style="text-transform:lowercase;font-variant:small-caps;">vii</span> emission lines were consistent with the observed ones within a factor of three in four out of the five cases except for an event in which a line-of-sight direction was toward the night side of the high-latitude magnetosheath and a major geomagnetic storm was observed. Those of O <span style="text-transform:lowercase;font-variant:small-caps;">viii</span> emission lines were underestimated by a factor of three or more in all five cases. On the other hand, the modeled O <span style="text-transform:lowercase;font-variant:small-caps;">vii</span> and O <span style="text-transform:lowercase;font-variant:small-caps;">viii</span> light curves reproduced the observed ones after being scaled by ratios between the observed and modeled average intensities. In particular, short-term variations due to line-of-sight directions traversing cusp regions during an orbital motion of the Suzaku satellite were reproduced. These results are discussed in the context of model uncertainties.</span></description>
137 <prism:volume xmlns:prism="prism">75</prism:volume>
138 <prism:number xmlns:prism="prism">1</prism:number>
139 <prism:startingPage xmlns:prism="prism">128</prism:startingPage>
140 <prism:endingPage xmlns:prism="prism">152</prism:endingPage>
141 <prism:doi xmlns:prism="prism">10.1093/pasj/psac095</prism:doi>
142 <guid>http://doi.org/10.1093/pasj/psac095</guid>
143 </item>
144 <item>
145 <title>Suzaku and Chandra study of diffuse X-ray emission from the massive star-forming region RCW 38</title>
146 <link>https://academic.oup.com/pasj/article/75/1/187/6887603?rss=1</link>
147 <pubDate>Mon, 12 Dec 2022 00:00:00 GMT</pubDate>
148 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>In some massive star-forming regions, diffuse X-ray emission has been observed. It can be classified as thermal emission from sub- or several-keV plasmas, non-thermal emission represented by the power law, or a mixture of them. We have studied the nearby (∼1.7 kpc) young massive star-forming region RCW 38. In a previous study, non-thermal diffuse X-ray emission of 1.25 × 1.75 pc (∼2${_{.}^{\prime}}$5 × 3${_{.}^{\prime}}$5) was reported from Chandra observation. We observed the same region for 72 ks with Suzaku which has a low background and is highly sensitive to spatially extended emission. To detect and consider point source contributions, we also used Chandra data. We divided the area according to the radius from the cluster center. In the inner region (<span style="font-style:italic;">r</span> &lt; 2${_{.}^{\prime}}$0), the existence of the non-thermal component (power law, Γ = 1.7 ± 0.4) was suggested although a two-temperature thermal model (<span style="font-style:italic;">kT</span> = 0.90 ± 0.07 and $6.2^{+7.7}_{-2.3}\:$keV) could not be rejected. In the outer region (<span style="font-style:italic;">r</span> = 2${_{.}^{\prime}}$0–5${_{.}^{\prime}}$5), a two-temperature (<span style="font-style:italic;">kT</span> = 0.95 ± 0.10 and 4.8 ± 0.6 keV) thermal plasma model was favorable. In this paper, the origin of the diffuse X-ray emission is discussed in the context of non-thermal/thermal emission and energetics.</span></description>
149 <prism:volume xmlns:prism="prism">75</prism:volume>
150 <prism:number xmlns:prism="prism">1</prism:number>
151 <prism:startingPage xmlns:prism="prism">187</prism:startingPage>
152 <prism:endingPage xmlns:prism="prism">198</prism:endingPage>
153 <prism:doi xmlns:prism="prism">10.1093/pasj/psac100</prism:doi>
154 <guid>http://doi.org/10.1093/pasj/psac100</guid>
155 </item>
156 <item>
157 <title>Modeling photometric variations due to a global inhomogeneity on an obliquely rotating star: Application to light curves of white dwarfs</title>
158 <link>https://academic.oup.com/pasj/article/75/1/103/6884610?rss=1</link>
159 <pubDate>Fri, 09 Dec 2022 00:00:00 GMT</pubDate>
160 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>We develop a general framework to compute photometric variations induced by the oblique rotation of a star with an axisymmetric inhomogeneous surface. We apply the framework to compute light curves of white dwarfs adopting two simple models of their surface inhomogeneity. Depending on the surface model and the location of the observer, the resulting light curve exhibits a departure from a purely sinusoidal curve that is observed for a fraction of white dwarfs. As a specific example, we fit our model to the observed phase-folded light curve of a fast-spinning white dwarf ZTF J190132.9+145808.7 (with a rotation period of 419 s). We find that the size and obliquity angle of the spot responsible for the photometric variation are Δθ<sub>s</sub> ≈ 60° and θ<sub>⋆</sub> ≈ 60° or 90°, respectively, implying an interesting constraint on the surface distribution of the magnetic field on white dwarfs.</span></description>
161 <prism:volume xmlns:prism="prism">75</prism:volume>
162 <prism:number xmlns:prism="prism">1</prism:number>
163 <prism:startingPage xmlns:prism="prism">103</prism:startingPage>
164 <prism:endingPage xmlns:prism="prism">119</prism:endingPage>
165 <prism:doi xmlns:prism="prism">10.1093/pasj/psac093</prism:doi>
166 <guid>http://doi.org/10.1093/pasj/psac093</guid>
167 </item>
168 <item>
169 <title>A close-in planet orbiting giant star HD 167768</title>
170 <link>https://academic.oup.com/pasj/article/75/1/169/6880842?rss=1</link>
171 <pubDate>Wed, 07 Dec 2022 00:00:00 GMT</pubDate>
172 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>We report the detection of a giant planet orbiting the G-type giant star HD 167768 from radial velocity measurements using the High Dispersion Echelle Spectrograph (HIDES) at Okayama Astrophysical Observatory (OAO). HD 167768 has a mass of $1.08_{-0.12}^{+0.14}\, M_{\odot }$, a radius of $9.70_{-0.25}^{+0.25}\, R_{\odot }$, a metallicity of $[\mbox{Fe}/\mbox{H}]=-0.67_{-0.08}^{+0.09}$, and a surface gravity of $\log g = 2.50_{-0.06}^{+0.06}$. The planet orbiting the star is a warm Jupiter, having a period of $20.6532_{-0.0032}^{+0.0032}\:\mbox{d}$, a minimum mass of $0.85_{-0.11}^{+0.12}\, M_{\rm {J}}$, and an orbital semimajor axis of $0.1512_{-0.0063}^{+0.0058}\:\mbox{au}$. The planet has one of the shortest orbital periods among those ever found around deeply evolved stars (log <span style="font-style:italic;">g</span> &lt; 3.5) using radial velocity methods. The equilibrium temperature of the planet is 1874 K, as high as a hot Jupiter. The radial velocities show two additional regular variations at 41 d and 95 d, suggesting the possibility of outer companions in the system. Follow-up monitoring will enable validation of the periodicity. We also calculated the orbital evolution of HD 167768 b and found that the planet will be engulfed within 0.15 Gyr.</span></description>
173 <prism:volume xmlns:prism="prism">75</prism:volume>
174 <prism:number xmlns:prism="prism">1</prism:number>
175 <prism:startingPage xmlns:prism="prism">169</prism:startingPage>
176 <prism:endingPage xmlns:prism="prism">176</prism:endingPage>
177 <prism:doi xmlns:prism="prism">10.1093/pasj/psac097</prism:doi>
178 <guid>http://doi.org/10.1093/pasj/psac097</guid>
179 </item>
180 <item>
181 <title>High-sensitivity VLBI observations of water masers in the Seyfert galaxy NGC 1068</title>
182 <link>https://academic.oup.com/pasj/article/75/1/71/6872751?rss=1</link>
183 <pubDate>Mon, 05 Dec 2022 00:00:00 GMT</pubDate>
184 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>We present observational results of water vapor maser emission with our high-sensitivity 22 GHz very long baseline interferometry (VLBI) imaging of the Seyfert galaxy NGC 1068. In this galaxy, there are the following four nuclear radio sources; NE, C, S1, and S2. Among them, the S1 component has been identified as the nucleus while the C component has been considered as attributed to the radio jet. In our VLBI observation, we find the following two types of water maser emission at the S1 component. One is a linearly aligned component that is considered as an edge-on disk with an inner radius of 0.62 pc. The dynamical mass enclosed within the inner radius was estimated to be 1.5 × 10<sup>7</sup> <span style="font-style:italic;">M</span><sub>⊙</sub> by assuming the circular Keplerian motion. Note, however, that the best-fitting rotation curve shows a sub-Keplerian rotation (<span style="font-style:italic;">v</span> ∝ <span style="font-style:italic;">r</span><sup>−0.24±0.10</sup>). The other is water maser emission distributed around the rotating disk component up to 1.5 pc from the S1 component, suggesting a bipolar outflow from the S1 component. Further, we detected water maser emission in the C component for the first time with VLBI, and discovered a ring-like distribution of water maser emission. It is known that a molecular cloud is associated with the C component (both HCN and HCO<sup>+</sup> emission lines are detected by ALMA). Therefore, the ring-like maser emission can be explained by the jet collision to the molecular cloud. However, if these ring-like water masing clouds constitute a rotating ring around the C component, it is likely that the C component also has a supermassive black hole with a mass of ∼10<sup>6</sup> <span style="font-style:italic;">M</span><sub>⊙</sub> that could be supplied from a past minor merger of a nucleated satellite galaxy.</span></description>
185 <prism:volume xmlns:prism="prism">75</prism:volume>
186 <prism:number xmlns:prism="prism">1</prism:number>
187 <prism:startingPage xmlns:prism="prism">71</prism:startingPage>
188 <prism:endingPage xmlns:prism="prism">81</prism:endingPage>
189 <prism:doi xmlns:prism="prism">10.1093/pasj/psac092</prism:doi>
190 <guid>http://doi.org/10.1093/pasj/psac092</guid>
191 </item>
192 <item>
193 <title>XMM-Newton view of the shock heating in an early merging cluster, CIZA J1358.9−4750</title>
194 <link>https://academic.oup.com/pasj/article/75/1/37/6862036?rss=1</link>
195 <pubDate>Thu, 01 Dec 2022 00:00:00 GMT</pubDate>
196 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>CIZA J1358.9−4750 is a nearby galaxy cluster in the early phase of a major merger. The two-dimensional temperature map using XMM-Newton EPIC-PN observation confirms the existence of a high-temperature region, which we call the “hot region,” in the “bridge region” connecting the two clusters. The ∼500 kpc wide region between the south-east and north-west boundaries also has higher pseudo-pressure compared to the unshocked regions, suggesting the existence of two shocks. The southern shock front is clearly visible in the X-ray surface brightness image and has already been reported by Kato et al. (2015, PASJ, 67, 71). The northern one, on the other hand, is newly discovered. To evaluate their Mach number, we constructed a three-dimensional toy merger model with overlapping shocked and unshocked components in the line of sight. The unshocked and pre-shock intracluster medium (ICM) conditions are estimated based on those outside the interacting bridge region, assuming point symmetry. The hot-region spectra are modeled with two-temperature thermal components, assuming that the shocked condition follows the Rankin–Hugoniot relation with the pre-shock condition. As a result, the shocked region is estimated to have a line-of-sight depth of ∼1 Mpc with a Mach number of ∼1.3 in the south-east shock and ∼1.7 in the north-west shock. The age of the shock waves is estimated to be ∼260 Myr. This three-dimensional merger model is consistent with the Sunyaev–Zel’dovich signal obtained using the Planck observation within the cosmic microwave background fluctuations. The total flow of the kinetic energy of the ICM through the south-east shock was estimated to be ∼2.2 × 10<sup>42</sup> erg s<sup>−1</sup>. Assuming that $10\%$ of this energy is converted into ICM turbulence, the line–of–sight velocity dispersion is calculated to be ∼200 km s<sup>−1</sup>, which is basically resolvable via upcoming high spectral resolution observations.</span></description>
197 <prism:volume xmlns:prism="prism">75</prism:volume>
198 <prism:number xmlns:prism="prism">1</prism:number>
199 <prism:startingPage xmlns:prism="prism">37</prism:startingPage>
200 <prism:endingPage xmlns:prism="prism">51</prism:endingPage>
201 <prism:doi xmlns:prism="prism">10.1093/pasj/psac087</prism:doi>
202 <guid>http://doi.org/10.1093/pasj/psac087</guid>
203 </item>
204 <item>
205 <title>Spatial structure and dynamical state of the old open cluster Collinder 261 based on a clustering method</title>
206 <link>https://academic.oup.com/pasj/article/75/1/82/6854448?rss=1</link>
207 <pubDate>Wed, 30 Nov 2022 00:00:00 GMT</pubDate>
208 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>In this paper, we investigate the memberships, spatial structure, and dynamical state of the old open cluster Collinder 261 (8 Gyr) based on Gaia-DR3 data. We develop a robust clustering method to calculate membership probabilities for 24858 sample stars within 20′ of the cluster center. We can identify 2619 likely cluster members (including 54 blue stragglers) down to <span style="font-style:italic;">G</span> ∼ 20 mag. We use a Monte Carlo simulation method to estimate a distance of 2909 ± 90 pc for the cluster based on 281 high-probability members (<span style="font-style:italic;">P</span> &gt; 0.9). We find that the detectable cluster radius (<span style="font-style:italic;">R</span><sub>cl</sub>) is at least 14′ (∼11.8 pc), which is much larger than previously thought. Based on the obtained cluster members, the core and tidal radii of the cluster are determined to be $R_{\rm c}={3{^{\prime }_{.}}4}\pm {0.1}$ (∼2.9 ± 0.1 pc) and $R_{\rm t}={19{^{\prime }_{.}}8}\pm {1{^{\prime }_{.}}9}$ (∼16.8 ± 1.6 pc), respectively. A concentration parameter of log (<span style="font-style:italic;">R</span><sub>t</sub>/<span style="font-style:italic;">R</span><sub>c</sub>) ∼0.76 is determined, indicating that Collinder 261 has formed a clear core–halo structure, but its spatial structure is much looser than the old open clusters M 67 (4 Gyr) and NGC 188 (7 Gyr). We also find that the membership probabilities are suitable for analyzing the mass segregation effect in the cluster. The orbit parameters show that Collinder 261 is moving along a near-circular orbit (<span style="font-style:italic;">e</span> ∼ 0.025) well inside the solar circle (<span style="font-style:italic;">R</span><sub>p</sub> ∼ 6.928 kpc, <span style="font-style:italic;">R</span><sub>a</sub> ∼ 7.285 kpc), and it can reach a maximum height of <span style="font-style:italic;">Z</span><sub>max</sub> ∼ 533 pc from the Galactic plane.</span></description>
209 <prism:volume xmlns:prism="prism">75</prism:volume>
210 <prism:number xmlns:prism="prism">1</prism:number>
211 <prism:startingPage xmlns:prism="prism">82</prism:startingPage>
212 <prism:endingPage xmlns:prism="prism">89</prism:endingPage>
213 <prism:doi xmlns:prism="prism">10.1093/pasj/psac091</prism:doi>
214 <guid>http://doi.org/10.1093/pasj/psac091</guid>
215 </item>
216 <item>
217 <title>The ultracompact regions G40.54+2.59 and G34.13+0.47: A new detection of compact radio sources†</title>
218 <link>https://academic.oup.com/pasj/article/75/1/90/6854447?rss=1</link>
219 <pubDate>Wed, 30 Nov 2022 00:00:00 GMT</pubDate>
220 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>We report the detection of three compact (&lt;0.001 pc) radio sources (CRSs) at the <span style="font-style:italic;">K</span><sub>a</sub>-band (0.9 cm) in the ultra-compact (UC) H <span style="text-transform:lowercase;font-variant:small-caps;">ii</span> regions G040.54+2.59 (two CRSs) and G034.13+0.47 (one CRS). These CRSs have weak flux densities and are located at the center of their respective UC H <span style="text-transform:lowercase;font-variant:small-caps;">ii</span> regions. We found no clear association between massive ionizing stars and CRSs but some radiative influence on the latter, as suggested by their large emission measures (&gt;10<sup>7</sup> cm<sup>−6</sup> pc), typical of photo-evaporating neutral objects close to or associated with massive stars. Our modelling of G40.54+2.59 shows that its CRSs supply enough ionized material to shape its morphology while significantly extending its observable lifetime. On the other hand, despite the possible relation of the CRS with the large-scale outflow signatures observed in G034.13+0.47, the influence of this CRS on the evolution of the UC H <span style="text-transform:lowercase;font-variant:small-caps;">ii</span> region is unlikely. Our results show that the presence of CRSs can alleviate the so-called lifetime problem of UC H <span style="text-transform:lowercase;font-variant:small-caps;">ii</span> regions. Still, to address the dynamical evolution of these regions adequately, the scenario must include additional mechanisms like ambient confinement, or the role of the kinematics of their associated stellar objects.</span></description>
221 <prism:volume xmlns:prism="prism">75</prism:volume>
222 <prism:number xmlns:prism="prism">1</prism:number>
223 <prism:startingPage xmlns:prism="prism">90</prism:startingPage>
224 <prism:endingPage xmlns:prism="prism">102</prism:endingPage>
225 <prism:doi xmlns:prism="prism">10.1093/pasj/psac090</prism:doi>
226 <guid>http://doi.org/10.1093/pasj/psac090</guid>
227 </item>
228 <item>
229 <title>The role of resistivity in hot accretion flows with anisotropic pressure: Comparing magnetic field models</title>
230 <link>https://academic.oup.com/pasj/article/75/1/52/6840005?rss=1</link>
231 <pubDate>Tue, 22 Nov 2022 00:00:00 GMT</pubDate>
232 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>In hot accretion flows, such as the accretion flow in the Galactic center (Sgr A*) and in M 87, the collisional mean free path of the charged particles is significantly larger than the typical length-scale of the accretion flows. Under these conditions, the pressure perpendicular to the magnetic field and that parallel to the magnetic field are not the same; therefore, the pressure is anisotropic to magnetic field lines. On the other hand, the resistivity as a dissipative mechanism plays a key role in the structure and the heating of hot accretion flows. In the present paper, we study the dynamics of resistive hot accretion flows with anisotropic pressure when the magnetic fields have even <span style="font-style:italic;">z</span>-symmetry about the midplane. By presenting a set of self-similar solutions, we find that if the magnetic fields have even <span style="font-style:italic;">z</span>-symmetry or the viscosity form depends on the strength of magnetic field, the disc properties can be entirely different. In the presence of symmetric fields, the velocity components and the disc temperature increase considerably. Also, we show that the increase in infall velocity and temperature due to the anisotropic pressure can be more significant if the resistivity is taken into account. Our results indicate that the resistivity can be an effective mechanism for the heating of hot accretion flows in the high-limit of the magnetic diffusivity parameter. Moreover, the heating due to the anisotropic pressure is comparable to the resistive heating, only when the strength of anisotropic pressure is about unity. The increase of disc temperature can lead to the acceleration of the electrons in such flows. This helps us to explain the origin of phenomena such as the flares in Sgr A*. Our results predict that the presence of resistivity makes it easier for outflows to launch from hot accretion flows.</span></description>
233 <prism:volume xmlns:prism="prism">75</prism:volume>
234 <prism:number xmlns:prism="prism">1</prism:number>
235 <prism:startingPage xmlns:prism="prism">52</prism:startingPage>
236 <prism:endingPage xmlns:prism="prism">70</prism:endingPage>
237 <prism:doi xmlns:prism="prism">10.1093/pasj/psac089</prism:doi>
238 <guid>http://doi.org/10.1093/pasj/psac089</guid>
239 </item>
240 <item>
241 <title>The microvariability and wavelength dependence of polarization degree/angle of BL Lacertae in the outburst 2020 to 2021</title>
242 <link>https://academic.oup.com/pasj/article/75/1/1/6825284?rss=1</link>
243 <pubDate>Sat, 12 Nov 2022 00:00:00 GMT</pubDate>
244 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>We have obtained simultaneous and continuous photo-polarization observations of the blazar BL Lacertae in optical and near-infrared (NIR) bands during an historical outburst from 2020 to 2021. In total, 14 nights of observations were performed where 10 observations show microvariability on timescales of a few minutes to several hours. This suggests a compact emission region, and the timescales are difficult to explain by a one-zone shock-in-jet model. Moreover, we found significant differences in the polarization degree (PD) and angle between optical and NIR bands. Nine nights showed a PD in the optical band that is greater than or equal to that in the NIR band, which can be explained by either a shock-in-jet model or the Turbulent Extreme Multi-Zone (TEMZ) model. On the other hand, five nights showed higher PD in an NIR band than an optical band, which cannot be explained by simple shock-in-jet models nor the simple TEMZ model. The observed timescales and wavelength-dependency of the PD and polarization angle suggest the existence of complicated multiple emission regions such as an irregular TEMZ model.</span></description>
245 <prism:volume xmlns:prism="prism">75</prism:volume>
246 <prism:number xmlns:prism="prism">1</prism:number>
247 <prism:startingPage xmlns:prism="prism">1</prism:startingPage>
248 <prism:endingPage xmlns:prism="prism">13</prism:endingPage>
249 <prism:doi xmlns:prism="prism">10.1093/pasj/psac084</prism:doi>
250 <guid>http://doi.org/10.1093/pasj/psac084</guid>
251 </item>
252 <item>
253 <title>X-ray spectroscopy of the accretion disk corona source 2S 0921−630 with Suzaku archival data</title>
254 <link>https://academic.oup.com/pasj/article/75/1/30/6825280?rss=1</link>
255 <pubDate>Sat, 12 Nov 2022 00:00:00 GMT</pubDate>
256 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>2S 0921−630 is an eclipsing low-mass X-ray binary (LMXB) with an orbital period of ∼9 d. Past X-ray observations have revealed that 2S 0921−630 has an extended accretion disk corona (ADC), from which most of the X-rays from the system are emitted. We report the result of our Suzaku archival data analysis of 2S 0921−630. The average X-ray spectrum is reproduced with a blackbody emission (<span style="font-style:italic;">kT</span><sub>bb</sub> ∼ 0.3 keV) Comptonized by optically thick gas (“Compton cloud”; optical depth τ ∼ 21) with a temperature of ∼2 keV, combined with 13 emission lines. We find that most of the emission lines correspond to highly ionized atoms: O, Ne, Mg, Si, S, Ar, and Fe. A Kα emission line and an absorption edge of semi-neutral iron (Fe textsci– textscxvii) are also detected. The semi-neutral iron Kα line is significantly broad, with a width of 0.11 ± 0.02 keV in sigma, which corresponds to the Doppler broadening by the Kepler motion at a radius of ∼10<sup>9</sup> cm. We suggest that the observed semi-neutral iron line originates at the inner part of the accretion disk in the immediate outside of the Compton cloud, i.e., the Compton cloud may have a radius of ∼10<sup>9</sup> cm.</span></description>
257 <prism:volume xmlns:prism="prism">75</prism:volume>
258 <prism:number xmlns:prism="prism">1</prism:number>
259 <prism:startingPage xmlns:prism="prism">30</prism:startingPage>
260 <prism:endingPage xmlns:prism="prism">36</prism:endingPage>
261 <prism:doi xmlns:prism="prism">10.1093/pasj/psac086</prism:doi>
262 <guid>http://doi.org/10.1093/pasj/psac086</guid>
263 </item>
264 <item>
265 <title>An empirical method for mitigating an excess up-scattering mass bias on the weak lensing mass estimates for shear-selected cluster samples</title>
266 <link>https://academic.oup.com/pasj/article/75/1/14/6819922?rss=1</link>
267 <pubDate>Thu, 10 Nov 2022 00:00:00 GMT</pubDate>
268 <description><span class="paragraphSection"><div class="boxTitle">Abstract</div>An excess up-scattering mass bias on a weak lensing cluster mass estimate is a statistical bias that an observed weak lensing mass (<span style="font-style:italic;">M</span><sub>obs</sub>) of a cluster of galaxies is, in a statistical sense, larger than its true mass (<span style="font-style:italic;">M</span><sub>true</sub>) because of a higher chance of up-scattering than that of down-scattering due to random noises in a weak lensing cluster shear profile. This non-symmetric scattering probability is caused by a monotonically decreasing cluster mass function with increasing mass. We examine this bias (defined by <span style="font-style:italic;">b</span> = <span style="font-style:italic;">M</span><sub>obs</sub>/<span style="font-style:italic;">M</span><sub>true</sub>) in weak lensing shear-selected clusters, and present an empirical method for mitigating it. In so doing, we perform the standard weak lensing mass estimate of realistic mock clusters, and find that the weak lensing mass estimate based on the standard χ<sup>2</sup> analysis gives a statistically correct confidence intervals, but resulting best-fitting masses are biased high on average. Our correction method uses the framework of the standard Bayesian statistics with the prior of the probability distribution of the cluster mass and concentration parameter from recent empirical models. We test our correction method using mock weak lensing clusters, and find that the method works well with resulting corrected <span style="font-style:italic;">M</span><sub>obs</sub>-bin averaged mass biases being close to unity within ${\sim}10\%$. We applied the correction method to weak lensing shear-selected cluster sample of Hamana, Shirasaki, and Lin (2020, PASJ, 72, 78), and present bias-corrected weak lensing cluster masses.</span></description>
269 <prism:volume xmlns:prism="prism">75</prism:volume>
270 <prism:number xmlns:prism="prism">1</prism:number>
271 <prism:startingPage xmlns:prism="prism">14</prism:startingPage>
272 <prism:endingPage xmlns:prism="prism">29</prism:endingPage>
273 <prism:doi xmlns:prism="prism">10.1093/pasj/psac085</prism:doi>
274 <guid>http://doi.org/10.1093/pasj/psac085</guid>
275 </item>
276 </channel>
277