魯迅的祖父周福淸攷 (十二) : 關於他的家系、生平及人物像

（十二）是第九章「被宣判“斬監侯”押進杭州府獄之後的周福淸（光緒十九年～光緒三十年）」。第九章的主要目的闡明被押進杭州的府獄之後的周福淸和周家的情況。第一節「獄中時代（光緒十九年～光緒二十七年）」：秋審，最初光緒二十年被認定情實犯因西太后還曆恩詔停勾，以後毎年予勾後改免勾牢固監侯，光緒二十六年因光緒帝三十歲詔停勾。周福淸坐牢當初非常緊張，但逐漸精神安定，光緒二十五年寫作家訓『恆訓』。長孫魯迅抄寫『恆訓』（這裏祇介紹原文。譯文別途要介紹）、周福淸詩集『桐華閣詩紗』（這兒只介紹原文）。第二節「從釋放到逝去（光緒二十七年～光緒三十年）」：光緒二十七年周福淸老朋友的刑部尚書薛允升援用光緒二十六年釋放亂中越獄後投首的官犯黃思永等的例，釋放周福淸了。二孫作人西興（杭州府蕭山縣）迎接他的祖父。周福淸回家後，馬上又開始諷刺大骂家屬等。同年族人周元祉從任地的陝西帶家屬回来。他得職是託周福淸的福的，他回郷後和周福淸經常閑聊，但是討厭周福淸常常提到族人某寡婦的艶史諷刺，以後雙方疏遠。同年二孫作人考進南京江南水師學堂。第二年長孫樹人留學日本。周福淸光緒三十年生病，臥病榻中他自作輓聯。同年六月一日他病死了（大夫又日何廉臣）。享年六十八歲。喪事因長孫樹人留學日本，二孫作人主持。雖然喪事基本上按照慣例，但是出席人寥寥。周福淸的妾潘氏宣統元年在蔣氏承認之下和周家斷絕關係。正室蔣氏宣統三年病死了，喪事長孫樹人按照矩主持（大夫又是何廉臣）

魯迅的祖父周福清攷 (七)関於他的家系,生平及人物像

（七）是第六章「内閣中書時代」全二節中的第二節「正式中書時代」的一部分（一「正式就任中書」中的（三）「正式中書周福清」、二「文郁的応考郷試」中的「応考郷試経歴」）。第二節的一中的（三）利用档案資料介紹周福清的正式中書時代的情况、応考同考官考試、応昇任調任的銓衡、擢升和公的収入等。周福清属于漢票簽処第二直房，主要従事草擬、校対中文票簽的工作，還有時兼任内閣誥勅房和中書科事務，還有時被派遣到内閣会典館、軍機処従事『清会典』、『方略』的編纂校対工作。順天府郷試和会試的同考官，内閣中書（正式的）也可以担任，周福清至少考了六次，都没考中。正式中書在任期内可以調任別処的中央官衙官唄或地方官，周福清応了両次宗人府漢堂主事的空額補充銓衡，但是第一次落選，第二次以感冒為借口缺席。周福清工作得既很謹慎又聡明，光緒十六年被擢升為内閣侍読代理見習。光緒十七年周福清捐納縮短試用期間，試用期間満了，得優等評語，决定做為地方官（同知）起用。光緒十八年吏部命周福清等応熱河（直隷省承徳府）州県官的銓衡，但是周福清又以感冒為借口缺席。其理由大概是周福清因江西知県時代嘗够苦頭，原来不想再当地方官吧。正式中書周福清的公収入只是俸銀年八十八両二十銭（候補中書中的両倍）俸米年十七石七斗（跟候補中書一様。一半発銀）和月二百文的公費（也跟候補中書一様），比候補中書時代多一点，但還過着很困難的生活。周福清的正式中書時代，児子文郁一共考了三次浙江郷試（光緒十四年戊子科、光緒十五己丑恩科、光緒十七年辛卯科），都没有通過。第二節的二提到文郁所応考的浙江郷試的監臨官等実行要員名単、試題、及格者和補缺者名単以及上海『申報』登載的関于浙江郷試的風聞等

Imaging Extended Emission-Line Regions of Obscured AGN with the Subaru Hyper Suprime-Cam Survey

Narrow-line regions excited by active galactic nuclei (AGN) are important for studying AGN photoionization and feedback. Their strong [O III] lines can be detected with broadband images, allowing morphological studies of these systems with large-area imaging surveys. We develop a new technique to reconstruct the [O III] images using the Subaru Hyper Suprime-Cam (HSC) Survey aided with spectra from the Sloan Digital Sky Survey (SDSS). The technique involves a careful subtraction of the galactic continuum to isolate emission from the [O III]$\lambda$5007 and [O III]$\lambda$4959 lines. Compared to traditional targeted observations, this technique is more efficient at covering larger samples with less dedicated observational resources. We apply this technique to an SDSS spectroscopically selected sample of 300 obscured AGN at redshifts 0.1 - 0.7, uncovering extended emission-line region candidates with sizes up to tens of kpc. With the largest sample of uniformly derived narrow-line region sizes, we revisit the narrow-line region size-luminosity relation. The area and radii of the [O III] emission-line regions are strongly correlated with the AGN luminosity inferred from the mid-infrared (15 $\mu$m rest-frame) with a power-law slope of $0.62^{+0.05}_{-0.06} \pm 0.10$ (statistical and systemic errors), consistent with previous spectroscopic findings. We discuss the implications for the physics of AGN emission-line region and future applications of this technique, which should be useful for current and next-generation imaging surveys to study AGN photoionization and feedback with large statistical samples.Comment: 20 pages, 13 figures, MNRAS submitte

A Wide and Deep Exploration of Radio Galaxies with Subaru HSC (WERGS). II. Physical Properties derived from the SED Fitting with Optical, Infrared, and Radio Data

We present physical properties of radio galaxies (RGs) with $f_{\rm 1.4 GHz} >$ 1 mJy discovered by Subaru Hyper Supreme-Cam (HSC) and VLA Faint Images of the Radio Sky at Twenty-Centimeters (FIRST) survey. For 1056 FIRST RGs at $0 < z \leq 1.7$ with HSC counterparts in about 100 deg$^2$, we compiled multi-wavelength data of optical, near-infrared (IR), mid-IR, far-IR, and radio (150 MHz). We derived their color excess ($E (B-V)_{*}$), stellar mass, star formation rate (SFR), IR luminosity, the ratio of IR and radio luminosity ($q_{\rm IR}$), and radio spectral index ($\alpha_{\rm radio}$) that are derived from the SED fitting with CIGALE. We also estimated Eddington ratio based on stellar mass and integration of the best-fit SEDs of AGN component. We found that $E (B-V)_{*}$, SFR, and IR luminosity clearly depend on redshift while stellar mass, $q_{\rm IR}$, and $\alpha_{\rm radio}$ do not significantly depend on redshift. Since optically-faint ($i_{\rm AB} \geq 21.3$) RGs that are newly discovered by our RG survey tend to be high redshift, they tend to not only have a large dust extinction and low stellar mass but also have high SFR and AGN luminosity, high IR luminosity, and high Eddington ratio compared to optically-bright ones. The physical properties of a fraction of RGs in our sample seem to differ from a classical view of RGs with massive stellar mass, low SFR, and low Eddington ratio, demonstrating that our RG survey with HSC and FIRST provides us curious RGs among entire RG population.Comment: 30 pages, 20 figures, and 4 tables, accepted for publication in ApJS. The catalog and SED template of radio galaxies will be accessible through an online servic

Subaru High-zz Exploration of Low-luminosity Quasars (SHELLQs). XVII. Black Hole Mass Distribution at z∼6z \sim 6 Estimated via Spectral Comparison with Low-zz Quasars

We report the distribution of black hole (BH) masses and Eddingont ratios estimated for a sample of 131 low luminosity quasars in the early cosmic epoch ($5.6 < z < 7.0$). Our work is based on Subaru High-$z$ Exploration of Low-Luminosity Quasars (SHELLQs) project, which has constructed a low luminosity quasar sample down to $M_{1450} \sim - 21$ mag, exploiting the survey data of Hyper Suprime-Cam installed on Subaru Telescope. The discovery spectra of these quasars are limited to the rest-frame wavelengths of $\sim$ 1200 -- 1400 \AA, which contains no emission lines that can be used as BH mass estimators. In order to overcome this problem, we made use of low-$z$ counterpart spectra from the Sloan Digital Sky Survey, which are spectrally matched to the high-$z$ spectra in overlapping wavelengths. We then combined the C~{\sc iv} emission line widths of the counterparts with the continuum luminosity from the SHELLQs data to estimate BH masses. The resulting BH mass distribution has a range of $\sim 10^{7-10} M_{\odot}$, with most of the quasars having BH masses $\sim 10^{8} M_{\odot}$ with sub-Eddington accretion. The present study provides not only a new insight into normal quasars in the reionization epoch, but also a new promising way to estimate BH masses of high-$z$ quasars without near-infrared spectroscopy.Comment: 18 pages, 17 figures, accepted for publication in Ap