Search

We have obtained three-dimensional maps of the universe in $\sim200\times200\times80$ comoving Mpc$^3$ (cMpc$^3$) volumes each at $z=5.7$ and $6.6$ based on a spectroscopic sample of 179 galaxies that achieves $\gtrsim80$\% completeness down to the Ly$\alpha$ luminosity of $\log(L_{\rm Ly\alpha}/[\mathrm{erg\ s^{-1}}])=43.0$, based on our Keck and Gemini observations and the literature. The maps reveal filamentary large-scale structures and two remarkable overdensities made out of at least 44 and 12 galaxies at $z=5.692$ (z57OD) and $z=6.585$ (z66OD), respectively, making z66OD the most distant overdensity spectroscopically confirmed to date with $>10$ spectroscopically confirmed galaxies. We compare spatial distributions of submillimeter galaxies at $z\simeq 4-6$ with our $z=5.7$ galaxies forming the large-scale structures, and detect a $99.97\%$ signal of cross correlation, indicative of a clear coincidence of dusty star-forming galaxy and dust unobscured galaxy formation at this early epoch. The galaxies in z57OD and z66OD are actively forming stars with star formation rates (SFRs) $\gtrsim5$ times higher than the main sequence, and particularly the SFR density in z57OD is 10 times higher than the cosmic average at the redshift (a.k.a. the Madau-Lilly plot). Comparisons with numerical simulations suggest that z57OD and z66OD are protoclusters that are progenitors of the present-day clusters with halo masses of $\sim10^{14}\ \mathrm{M_\odot}$., Comment: 17 pages, 11 figures, Accepted for Publication in ApJ

The implementation of allergen immunotherapy (AIT) requires extensive knowledge of allergen distribution in the region to identify high-risk regions for AIT utilization. However, the geographical distribution patterns of the major Dermatophagoides allergens in China remain unclear despite the increasing prevalence of these allergens.We performed comprehensive database searches of articles demonstrating the distribution patterns of Dermatophagoides-sensitized allergic rhinitis (AR) and allergic asthma (AA) in China, published between 1990 and 2017.We retrieved 163 articles encompassing 114,302 allergen-positive cases to generate the distribution maps. The rate of sensitization to Dermatophagoides pteronyssinus(D. pteronyssinus)and Dermatophagoides farinae (D. farinae) was similar in patients with AR (75.1 vs. 75.2%, p0.05) but not in those with AA (78.5 vs. 77.7%, p = 0.041). Patients with AR and AA shared similar regional distribution patterns of both D. pteronyssinus and D. farinae sensitization, which were highest in the southern and central parts of China and lowest in the northern regions, especially in the Northwest. The overall rate of sensitization to D. pteronyssinus and D. farinae was significantly higher in patients with AA (p0.001). Additionally, the annual mean temperature and humidity were the 2 major determinants of D. pteronyssinus and D. farinae sensitization in AR and of D. pteronyssinus sensitization in AA, whereas the annual mean temperature was the sole determinant for D. farinae sensitization in AA.These findings may inform clinicians of the strategies for the prevention of Dermatophagoides sensitization and may be of benefit to the future clinical management of allergic diseasesassociated with sensitization to Dermatophagoides mites.

We present far-infrared (FIR) properties of an extremely luminous infrared galaxy (ELIRG) at $z_{\rm spec}$ = 3.703, WISE J101326.25+611220.1 (WISE1013+6112). This ELIRG is selected as an IR-bright dust-obscured galaxy (DOG) based on the photometry from the Sloan digital sky survey (SDSS) and wide-field infrared survey explorer (WISE). In order to derive its accurate IR luminosity, we perform follow-up observations at 89 and 154 $\mu$m using the high-resolution airborne wideband camera-plus (HAWC+) on board the 2.7-m stratospheric observatory for infrared astronomy (SOFIA) telescope. We conduct spectral energy distribution (SED) fitting with CIGALE using 15 photometric data (0.4-1300 $\mu$m). We successfully pin down FIR SED of WISE1013+6112 and its IR luminosity is estimated to be $L_{\rm IR}$ = (1.62 $\pm$ 0.08) $\times 10^{14}$ $L_{\odot}$, making it one of the most luminous IR galaxies in the universe. We determine the dust temperature of WISE1013+6112 is $T_{\rm dust}$ = 89 $\pm$ 3 K, which is significantly higher than that of other populations such as SMGs and FIR-selected galaxies at similar IR luminosities. The resultant dust mass is $M_{\rm dust}$ = (2.2 $\pm$ 0.1) $\times 10^{8}$ $M_{\odot}$. This indicates that WISE1013+6112 has a significant active galactic nucleus (AGN) and star-forming activity behind a large amount of dust., Comment: 9 pages, 4 figures, and 2 tables, accepted for publication in ApJ

We report detections of two 1.2 mm continuum sources (S 1.2 mm ∼ 0.6 mJy) without any counterparts in the deep H- and/or K-band image (i.e., K-band magnitude ≳26 mag). These near-infrared-dark faint millimeter sources are uncovered by ASAGAO, a deep and wide-field (≃26 arcmin2) Atacama Large Millimeter/submillimeter Array (ALMA) 1.2 mm survey. One has a red IRAC (3.6 and 4.5 μm) counterpart, and the other has been independently detected at 850 and 870 μm using SCUBA2 and ALMA Band 7, respectively. Their optical-to-radio spectral energy distributions indicate that they can lie at z ≳ 3–5 and can be in the early phase of massive galaxy formation. Their contribution to the cosmic star formation rate density is estimated to be ∼1 × 10‑3 M ⊙ yr‑1 Mpc‑3 if they lie somewhere in the redshift range of z ∼ 3–5. This value can be consistent with, or greater than, that of bright submillimeter galaxies (S 870 μm > 4.2 mJy) at z ∼ 3–5. We also uncover three more candidate near-infrared-dark faint ALMA sources without any counterparts (S 1.2 mm ∼ 0.45–0.86 mJy). These results show that an unbiased ALMA survey can reveal the dust-obscured star formation activities, which were missed in previous deep optical/near-infrared surveys.

We identify multi-wavelength counterparts to 1,147 submillimeter sources from the S2COSMOS SCUBA-2 survey of the COSMOS field by employing a recently developed radio$+$machine-learning method trained on a large sample of ALMA-identified submillimeter galaxies (SMGs), including 260 SMGs identified in the AS2COSMOS pilot survey. In total, we identify 1,222 optical/near-infrared(NIR)/radio counterparts to the 897 S2COSMOS submillimeter sources with S$_{850}$>1.6mJy, yielding an overall identification rate of ($78\pm9$)%. We find that ($22\pm5$)% of S2COSMOS sources have multiple identified counterparts. We estimate that roughly 27% of these multiple counterparts within the same SCUBA-2 error circles very likely arise from physically associated galaxies rather than line-of-sight projections by chance. The photometric redshift of our radio$+$machine-learning identified SMGs ranges from z=0.2 to 5.7 and peaks at $z=2.3\pm0.1$. The AGN fraction of our sample is ($19\pm4$)%, which is consistent with that of ALMA SMGs in the literature. Comparing with radio/NIR-detected field galaxy population in the COSMOS field, our radio+machine-learning identified counterparts of SMGs have the highest star-formation rates and stellar masses. These characteristics suggest that our identified counterparts of S2COSMOS sources are a representative sample of SMGs at z, 24 pages, 14 figures, 3 tables, resubmitted to ApJ

Objectives To assess the prognostic role of hepatitis in pediatric patients with aplastic anemia and the incidence of hepatitis B among patients with hepatitis-associated aplastic anemia in an area with a previously high prevalence of hepatitis B after nationwide hepatitis B vaccination for 30 years. Study design Pediatric patients (n = 78) with aplastic anemia were enrolled in this study, including 9 with hepatitis-associated aplastic anemia. We collected the clinical characteristics, etiologies of the aplastic anemia, hepatitis B virus serology and serum hepatitis B viral load, response to the treatments, and survival outcome from the participants. We applied univariate and multivariate Cox regression analysis to evaluate the correlations between clinical features and survival outcome. Survival analysis was done using Cox regression model and Kaplan-Meier curves. Results Patients with hepatitis-associated aplastic anemia were related to significantly worse survival prognosis when compared with patients with non-hepatitis-associated aplastic anemia, and hepatitis-associated aplastic anemia was the only independent prognostic factor to predict a poor survival outcome in our patients with aplastic anemia by multivariable analysis. In none of the total 78 patients was aplastic anemia related to hepatitis B virus infection. Conclusions Patients with hepatitis-associated aplastic anemia had a significantly worse prognosis when compared with patients whose aplastic anemia was not hepatitis-associated. This study demonstrates the potential benefit of hepatitis B vaccination in decreasing the incidence of hepatitis-associated aplastic anemia in children.

Rising worldwide cancer incidence and resistance to current anti-cancer drugs necessitate the need for new pharmaceutical compounds and drug delivery system. Two novel series of biscoumarin (1-4) and dihydropyran (5-16) derivatives were synthesized via a one-pot multicomponent condensation reaction and evaluated for their antitumor activity in vitro. The X-ray crystal structure analysis of four representative compounds 2, 7, 10 and 13 confirmed the structures of these compounds. Compounds 1-4 showed the most potent antitumor activity among the total 16 derivatives. More interestingly, preliminary mechanism studies revealed that the most potent compound 4 induced apoptosis and arrested the cell cycle at the S phase in HUTU80 cells. Additionally, the increased accumulation of HUTU80 cells in the sub G1 peak further pointed to the occurence of the cell apoptosis. The selectivity index analysis demonstrated that all the biscoumarin compounds (SI=3.1-7.5) possess higher selectivity towards intestinal epithelial adenocarcinoma cell line (HuTu80) than positive control drug carboplatin (SI=1.6-1.8). The biscoumarin compounds also showed no obvious acute toxicity on mice.

Two series of biscoumarin (1-3) and dihydropyran (4-12) derivatives were successfully synthesized as new antitumor and antibacterial agents. The molecular structures of four representative compounds 2, 4, 7 and 10 were confirmed by single crystal X-ray diffraction study. The synthesized compounds (1-12) were evaluated for their antitumor activities against human intestinal epithelial adenocarcinoma cell line (HuTu80), mammary adenocarcinoma cell line (4T1) and pancreatic cancer cell line (PANC1) and antibacterial activities against one drug-sensitive Staphylococcus aureus (S. aureus ATCC 29213) strain and three MRSA strains (MRSA XJ 75302, Mu50, USA 300 LAC). The further mechanism study demonstrated that the most potent compound 1 could obviously inhibit the proliferation of cancer cells via the mechanism to induce apoptosis.

We present rest-frame far-infrared (FIR) and optical size measurements of AGN hosts and star-forming galaxies in the COSMOS field, enabled by high-resolution ALMA/1 mm (0.1 arcsec - 0.4 arcsec) and HST/F814W imaging (~ 0.1 arcsec). Our sample includes 27 galaxies at z, accepted for publication in ApJ

We report the discovery of a Compton-thick (CT) dust-obscured galaxy (DOG) at $z$ = 0.89, WISE J082501.48+300257.2 (WISE0825+3002), observed by Nuclear Spectroscopic Telescope Array (NuSTAR). X-ray analysis with the XCLUMPY model revealed that hard X-ray luminosity in the rest-frame 2-10 keV band of WISE0825+3002 is $L_{\rm X}$ (2-10 keV) = $4.2^{+2.8}_{-1.6} \times 10^{44}$ erg s$^{-1}$ while its hydrogen column density is $N_{\rm H}$ = $1.0^{+0.8}_{-0.4} \times 10^{24}$ cm$^{-2}$, indicating that WISE0825+3002 is a mildly CT active galactic nucleus (AGN). We performed the spectral energy distribution (SED) fitting with CIGALE to derive its stellar mass, star formation rate, and infrared luminosity. The estimated Eddington ratio based on stellar mass and integration of the best-fit SED of AGN component is $\lambda_{\rm Edd}$ = 0.70, which suggests that WISE0825+3002 harbors an actively growing black hole behind a large amount of gas and dust. We found that the relationship between luminosity ratio of X-ray and 6 $\mu$m, and Eddington ratio follows an empirical relation for AGNs reported by Toba et al. (2019a)., Comment: 10 pages, 7 figures, and 2 tables, accepted for publication in ApJ

We present the survey design, data reduction, construction of images, and source catalog of the Atacama Large Millimeter/submillimeter Array (ALMA) twenty-six arcmin^2 survey of GOODS-S at one-millimeter (ASAGAO). ASAGAO is a deep (1sigma ~ 61 uJy/beam for a 250 klambda-tapered map with a synthesized beam size of 0.51" x 0.45") and wide area (26 arcmin^2) survey on a contiguous field at 1.2 mm. By combining with ALMA archival data in the GOODS-South field, we obtained a deeper map in the same region (1sigma ~ 30 uJy/beam for a deep region with a 250 klambda-taper, and a synthesized beam size of 0.59" x 0.53"), providing the largest sample of sources (25 sources at >=5.0sigma, 45 sources at >=4.5sigma) among ALMA blank-field surveys to date. The number counts shows that 52(+11 -8)% of the extragalactic background light at 1.2 mm is resolved into discrete sources at S1.2m > 135 uJy. We create infrared (IR) luminosity functions (LFs) in the redshift range of z = 1-3 from the ASAGAO sources with KS-band counterparts, and constrain the faintest luminosity of the LF at 2.0 < z < 3.0. The LFs are consistent with previous results based on other ALMA and SCUBA-2 observations, which suggest a positive luminosity evolution and negative density evolution with increasing redshift. We find that obscured star-formation of sources with IR luminosities of log(L(IR)/Lsun)} ~> 11.8 account for ~~60%-90% of the z ~ 2 cosmic star-formation rate density., 19 pages, 18 figures, accepted for publication in PASJ

We present the discovery of an extremely-luminous dust-obscured galaxy (DOG) at $z_{\rm spec}$ = 3.703, WISE J101326.25+611220.1. This DOG is selected as a candidate of extremely-luminous infrared (IR) galaxies based on the photometry from the Sloan Digital Sky Survey and Wide-field Infrared Survey Explorer. In order to derive its accurate IR luminosity, we perform follow-up observations at 450 and 850 $\mu$m using the Submillimetre Common User Bolometer Array 2 on the James Clerk Maxwell Telescope, and at 870 and 1300 $\mu$m using the Submillimeter Array, which enable us to pin down its IR Spectral Energy Distribution (SED). We perform SED fitting using 14 photometric data (0.4 - 1300 $\mu$m) and estimate its IR luminosity, $L_{\rm IR}$ (8-1000 $\mu$m), to be $2.2^{+1.5}_{-1.0}$ $\times 10^{14}$ $L_{\odot}$, making it one of the most luminous IR galaxies in the Universe. The energy contribution from an active galactic nucleus (AGN) to the IR luminosity is $94^{+6}_{-20}$%, which indicates it is an AGN-dominated DOG. On the other hand, its stellar mass ($M_*$) and star formation rate (SFR) are $\log \,(M_\ast/M_{\odot})$ = $11.2^{+0.6}_{-0.2}$ and $\log \,({\rm SFR}/M_{\odot}\,{\rm yr}^{-1}$) = $3.1^{+0.2}_{-0.1}$, respectively, which means that this DOG can be considered as a starburst galaxy in $M_*$--SFR plane. This extremely-luminous DOG shows significant AGN and star forming activity that provides us an important laboratory to probe the maximum phase of the co-evolution of galaxies and supermassive black holes., Comment: 10 pages, 6 figures, and 1 table, accepted for publication in ApJ

We analyze the >4-sigma sources in the most sensitive 100 arcmin^2 area (rms 4.5-sigma) obtained from high-resolution interferometric follow-up observations. The SCUBA-2---and hence ALMA---samples should be complete to 2.25 mJy. Of the 53 SCUBA-2 sources in this complete sample, only five have no ALMA detections, while 13% (68% confidence range 7-19%) have multiple ALMA counterparts. Color-based high-redshift dusty galaxy selection techniques find at most 55% of the total ALMA sample. In addition to using literature spectroscopic and optical/NIR photometric redshifts, we estimate FIR photometric redshifts based on an Arp 220 template. We identify seven z>4 candidates. We see the expected decline with redshift of the 4.5 micron and 24 micron to 850 micron flux ratios, confirming these as good diagnostics of z>4 candidates. We visually classify 52 ALMA sources, finding 44% (68% confidence range 35-53%) to be apparent mergers. We calculate rest-frame 2-8 keV and 8-28 keV luminosities using the 7 Ms Chandra X-ray image. Nearly all of the ALMA sources detected at 0.5-2 keV are consistent with a known X-ray luminosity to 850 micron flux relation for star-forming galaxies, while most of those detected at 2-7 keV are moderate luminosity AGNs that lie just above the 2-7 keV detection threshold. The latter largely have substantial obscurations of log N_H = 23-24 cm^-2, but two of the high-redshift candidates may even be Compton thick., 44 pages, 35 figures. Submitted to ApJ

We present a near-infrared (NIR) spectrum of WISE J1042+1641, an extremely red dust-obscured galaxy (DOG), which has been observed with the LIRIS on the 4.2m William Hershel Telescope. This object was selected as a hyper-luminous DOG candidate at z ~ 2 by combining the optical and IR photometric data based on the SDSS and WISE, although its redshift had not yet been confirmed. Based on the LIRIS observation, we confirmed its redshift of 2.521 and total IR luminosity of log(L_IR/L_sun) = 14.57, which satisfies the criterion for an extremely luminous IR galaxy (ELIRG). Moreover, we indicate that this object seems to have an extremely massive black hole with M_BH = 10^10.92 M_sun based on the broad Halpha line: the host stellar mass is derived as M_star = 10^13.55 M_sun by a fit of the spectral energy distribution. Very recently, it has been reported that this object is an anomalous gravitationally lensed quasar based on near-IR high-resolution imaging data obtained with the Hubble Space Telescope. Its magnification factor has also been estimated with some uncertainty (i.e., mu = 53-122). We investigate the ratio of the black hole to galaxy mass, which is less strongly affected by a lensing magnification factor, instead of the absolute values of the luminosities and masses. We find that the M_BH/M_star ratio (i.e., 0.0140-0.0204) is significantly higher than the local relation, following a sequence of unobscured quasars instead of obscured objects (e.g., submillimeter galaxies) at the same redshift. Moreover, the LIRIS spectrum shows strongly blueshifted oxygen lines with an outflowing velocity of ~ 1100 km/s, and our Swift X-ray observation also supports that this source is an absorbed AGN with an intrinsic column density of N_H = 4.9 x 10^23 cm^-2. These results imply that WISE J1042+1641 is in a blow-out phase at the end of the buried rapid black hole growth., Comment: 6 pages, 4 figures, accepted for publication in A&A

We report on a sensitive search for redshifted Hα line-emission from three high-metallicity damped Lyα absorbers (DLAs) at z ≈ 2.4 with the Near-infrared Integral Field Spectrometer (NIFS) on the Gemini-North telescope, assisted by the ALTtitude conjugate Adaptive optics for the InfraRed (ALTAIR) system with a laser guide star. Within the NIFS field-of-view, ≈3.22 arcsec × 2.92 arcsec corresponding to ≈25 kpc × 23 kpc at z = 2.4, we detect no statistically significant line-emission at the expected redshifted Hα wavelengths. The measured root-mean-square noise fluctuations in 0.4 arcsec apertures are 1–3 × 10-18 erg s-1 cm-2.

In this third paper of the Hawaii SCUBA-2 Lensing Cluster Survey series, we present Submillimeter Array (SMA) detections of six intrinsically faint 850 $\mu$m sources detected in SCUBA-2 images of the lensing cluster fields, A1689, A2390, A370, MACS J0717.5+3745, and MACS J1423.8+2404. Two of the SCUBA-2 sources split into doublets, yielding a total of eight SMA detections. The intrinsic 870 $\mu$m flux densities of these submillimeter galaxies (SMGs) are $\sim$ 1 mJy. Five of the eight SMGs are not detected in optical or near-infrared (NIR) images. The NIR-to-submillimeter flux ratios of these faint SMGs suggest that most of them are extremely dusty and/or at very high redshifts. Combining these SMGs and several other samples from the literature, we find a bimodal distribution for the faint sources in the space of submillimeter flux versus NIR-to-submillimeter flux ratio. While most of the SMA-detected lensed sources are very obscured, the other SMGs with similar flux densities are mostly bright in the NIR. Future ALMA observations of a large sample of SCUBA-2 sources in cluster fields will allow us to decide whether the bimodality we observe here really exists., Comment: 9 pages, 4 figures, 6 tables. Accepted for publication in ApJ

Hyper Suprime-Cam (HSC) is a wide-field imaging camera on the prime focus of the 8.2m Subaru telescope on the summit of Maunakea in Hawaii. A team of scientists from Japan, Taiwan and Princeton University is using HSC to carry out a 300-night multi-band imaging survey of the high-latitude sky. The survey includes three layers: the Wide layer will cover 1400 deg$^2$ in five broad bands ($grizy$), with a $5\,\sigma$ point-source depth of $r \approx 26$. The Deep layer covers a total of 26~deg$^2$ in four fields, going roughly a magnitude fainter, while the UltraDeep layer goes almost a magnitude fainter still in two pointings of HSC (a total of 3.5 deg$^2$). Here we describe the instrument, the science goals of the survey, and the survey strategy and data processing. This paper serves as an introduction to a special issue of the Publications of the Astronomical Society of Japan, which includes a large number of technical and scientific papers describing results from the early phases of this survey., Comment: 14 pages, 7 figures, 5 tables. Corrected for a typo in the coordinates of HSC-Wide spring equatorial field in Table 5

The identification of high-redshift massive galaxies with old stellar populations may pose challenges to some models of galaxy formation. However, to securely classify a galaxy as quiescent, it is necessary to exclude significant ongoing star formation, something that can be challenging to achieve at high redshift. In this letter, we analyse deep ALMA/870um and SCUBA-2/450um imaging of the claimed "post-starburst" galaxy ZF-20115 at z=3.717 that exhibits a strong Balmer break and absorption lines. The far-infrared imaging reveals a luminous starburst located 0.4+/-0.1 arcsec (~3kpc in projection) from the position of the rest-frame ultra-violet/optical emission, with an obscured star-formation rate of 100 Mo/yr. This star-forming component is undetected in the rest-frame ultraviolet but contributes significantly to the lower angular resolution photometry at restframe wavelengths >3500A, significantly complicating the determination of a reliable stellar mass. Importantly, in the presence of dust obscuration, strong Balmer features are not a unique signature of a post-starburst galaxy and are indeed frequently observed in infrared-luminous galaxies. We conclude that the ZF20015 system does not pose a challenge to current models of galaxy formation and that deep sub-/millimeter observations are a prerequisite for any claims of quiescence. The multi-wavelength observations of ZF20115 unveil a complex system with an intricate and spatially-varying star-formation history. ZF20115 demonstrates that understanding high-redshift obscured starbursts will only be possible with multi-wavelength studies that include high-resolution observations, available with the JWST, at mid-infrared wavelengths., ApJ submitted. Comments welcome

In this first paper in the SUPER GOODS series on powerfully star-forming galaxies in the two GOODS fields, we present a deep SCUBA-2 survey of the GOODS-N at both 850 and 450 micron (central rms noise of 0.28 mJy and 2.6 mJy, respectively). In the central region the 850 micron observations cover the GOODS-N to near the confusion limit of ~1.65 mJy, while over a wider 450 arcmin^2 region---well complemented by Herschel far-infrared imaging---they have a median 4-sigma limit of 3.5 mJy. We present >4-sigma catalogs of 186 850 micron and 31 450 micron selected sources. We use interferometric observations from the SMA and the VLA to obtain precise positions for 114 SCUBA-2 sources (28 from the SMA, all of which are also VLA sources). We present new spectroscopic redshifts and include all existing spectroscopic or photometric redshifts. We also compare redshifts estimated using the 20 cm to 850 micron and the 250 micron to 850 micron flux ratios. We show that the redshift distribution increases with increasing flux, and we parameterize the dependence. We compute the star formation history and the star formation rate (SFR) density distribution functions in various redshift intervals, finding that they reach a peak at z=2-3 before dropping to higher redshifts. We show that the number density per unit volume of SFR>500 solar mass per year galaxies measured from the SCUBA-2 sample does not change much relative to that of lower SFR galaxies from UV selected samples over z=2-5, suggesting that, apart from changes in the normalization, the shape in the number density as a function of SFR is invariant over this redshift interval., Accepted for publication in ApJ. 38 pages, 26 figures

We report the discovery of an infrared (IR)-bright dust-obscured galaxy (DOG) that shows a strong ionized-gas outflow but no significant molecular gas outflow. Based on detail analysis of their optical spectra, we found some peculiar IR-bright DOGs that show strong ionized-gas outflow ([OIII]$\lambda$5007) from the central active galactic nucleus (AGN). For one of these DOGs (WISE J102905.90+050132.4) at $z_{\rm spec} = 0.493$, we performed follow-up observations using ALMA to investigate their CO molecular gas properties. As a result, we successfully detected $^{12}$CO($J$=2-1) and $^{12}$CO($J$=4-3) lines, and the continuum of this DOG. The intensity-weighted velocity map of both lines shows a gradient, and the line profile of those CO lines is well-fitted by a single narrow Gaussian, meaning that this DOG has no sign of strong molecular gas outflow. The IR luminosity of this object is $\log\,(L_{\rm IR}/L_{\odot})$ = 12.40 that is classified as ultraluminous IR galaxy (ULIRG). We found that (i) the stellar mass and star-formation rate relation and (ii) the CO luminosity and far-IR luminosity relation are consistent with those of typical ULIRGs at similar redshifts. These results indicate that the molecular gas properties of this DOG are normal despite that its optical spectrum showing a powerful AGN outflow. We conclude that a powerful ionized-gas outflow caused by the AGN does not necessarily affect the cold interstellar medium in the host galaxy at least for this DOG., Comment: 8 pages, 5 figures, and 1 table, accepted for publication in ApJ

We present the ionized gas properties of infrared (IR)-bright dust-obscured galaxies (DOGs) that show an extreme optical/IR color, $(i - [22])_{\rm AB} > 7.0$, selected with the Sloan Digital Sky Survey (SDSS) and Wide-field Infrared Survey Explorer (WISE). For 36 IR-bright DOGs that show [OIII]$\lambda$5007 emission in the SDSS spectra, we performed a detailed spectral analysis to investigate their ionized gas properties. In particular, we measured the velocity offset (the velocity with respect to the systemic velocity measured from the stellar absorption lines) and the velocity dispersion of the [OIII] line. We found that the derived velocity offset and dispersion of most IR-bright DOGs are larger than those of Seyfert 2 galaxies (Sy2s) at $z < 0.3$, meaning that the IR-bright DOGs show relatively strong outflows compared to Sy2s. This can be explained by the difference of IR luminosity contributed from active galactic nucleus, $L_{\rm IR}$ (AGN), because we found that (i) $L_{\rm IR}$ (AGN) correlates with the velocity offset and dispersion of [OIII] and (ii) our IR-bright DOGs sample has larger $L_{\rm IR}$ (AGN) than Sy2s. Nevertheless, the fact that about 75% IR-bright DOGs have a large ($>$ 300 km s$^{-1}$) velocity dispersion, which is a larger fraction compared to other AGN populations, suggests that IR-bright DOGs are good laboratories to investigate AGN feedback. The velocity offset and dispersion of [OIII] and [NeIII]$\lambda$3869 are larger than those of [OII]$\lambda$3727, which indicates that the highly ionized gas tends to show more stronger outflows., Comment: 19 pages, 16 figures, and 2 tables, accepted for publication in ApJ

We investigate the star forming activity of a sample of infrared (IR)-bright dust-obscured galaxies (DOGs) that show an extreme red color in the optical and IR regime, $(i - [22])_{\rm AB} > 7.0$. Combining an IR-bright DOG sample with the flux at 22 $��$m $>$ 3.8 mJy discovered by Toba & Nagao (2016) with IRAS faint source catalog version 2 and AKARI far-IR (FIR) all-sky survey bright source catalog version 2, we selected 109 DOGs with FIR data. For a subsample of 7 IR-bright DOGs with spectroscopic redshift ($0.07 < z < 1.0$) that was obtained from literature, we estimated their IR luminosity, star formation rate (SFR), and stellar mass based on the spectral energy distribution fitting. We found that (i) WISE 22 $��$m luminosity at observed frame is a good indicator of IR luminosity for IR-bright DOGs and (ii) the contribution of active galactic nucleus (AGN) to IR luminosity increases with IR luminosity. By comparing the stellar mass and SFR relation for our DOG sample and literature, we found that most of IR-bright DOGs lie significantly above the main sequence of star-forming galaxies at similar redshift, indicating that the majority of IRAS- and/or AKARI-detected IR-bright DOGs are starburst galaxies., 12 pages, 8 figures, and 1 table, accepted for publication in ApJ

We present a study of the connection between black hole accretion, star formation, and galaxy morphology at z, Accepted for publication in ApJS

We present a multi-wavelength catalog in the Subaru-XMM Deep Field (SXDF) as part of the Spitzer Large Area Survey with Hyper-Suprime-Cam (SPLASH). We include the newly acquired optical data from the Hyper-Suprime Cam Subaru Strategic Program, accompanied by IRAC coverage from the SPLASH survey. All available optical and near-infrared data is homogenized and resampled on a common astrometric reference frame. Source detection is done using a multi-wavelength detection image including the $u$-band to recover the bluest objects. We measure multi-wavelength photometry and compute photometric redshifts as well as stellar masses for $\sim$1.17 million objects over $\sim$4.2 deg$^2$ with $\sim$800,000 objects in the 2.4 deg$^2$ HSC-UltraDeep coverage. Using the available spectroscopic redshifts from various surveys over the range of $0, Comment: 23 pages, 15 figures; accepted for publication in ApJS; comments welcome

The objective of this paper is to provide the references through finite element analysis for steel tube concrete beams bearing capacity settlement. The paper verified the correctness of the constitutive relation of concrete, the correctness and the model through the establishment of the concrete damaged plasticity model with recycled concrete details in the finite element analysis software ABAQUS. Then the stress characteristics of steel pipe concrete beam in bending condition under different substitution rate could be found through model calculation. The result is that the mid span bending - strain curve from simulation agreed to the experimental results, and the model is proved correct. Finally it came to the conclusions. Other things being equal, the recycled concrete filled square tube changed a lot in bending state when the substitution rate grows, but it didn’t occur to the circular one. In the meantime, the writer proposed the conjecture on the bearing capacity calculation of the two types of structure.

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 service

We present deep $J$ and $H$-band images in the extended Great Observatories Origins Deep Survey-North (GOODS-N) field covering an area of 0.22 $\rm{deg}^{2}$. The observations were taken using WIRCam on the 3.6-m Canada France Hawaii Telescope (CFHT). Together with the reprocessed $K_{\rm s}$-band image, the $5\sigma$ limiting AB magnitudes (in 2" diameter apertures) are 24.7, 24.2, and 24.4 AB mag in the $J$, $H$, and $K_{\rm s}$ bands, respectively. We also release a multi-band photometry and photometric redshift catalog containing 93598 sources. For non-X-ray sources, we obtained a photometric redshift accuracy $\sigma_{\mathrm{NMAD}}=0.036$ with an outlier fraction $\eta = 7.3\%$. For X-ray sources, which are mainly active galactic nuclei (AGNs), we cross-matched our catalog with the updated 2M-CDFN X-ray catalog from Xue et al. (2016) and found that 658 out of 683 X-ray sources have counterparts. $GALEX$ UV data are included in the photometric redshift computation for the X-ray sources to give $\sigma_{\mathrm{NMAD}} = 0.040$ with $\eta=10.5\%$. Our approach yields more accurate photometric redshift estimates compared to previous works in this field. In particular, by adopting AGN-galaxy hybrid templates, our approach delivers photometric redshifts for the X-ray counterparts with fewer outliers compared to the 3D-HST catalog, which fit these sources with galaxy-only templates.

Reinforced concrete eccentric frame - shear wall structures has been widely used in Engineering, but this structure is mostly used for high-rise structure. Depending on experimental study will be unable to accurately draw the seismic reflection of structure, it needs to use the simulation software to study the seismic performance of high-rise structure. In this paper, by using ANSYS finite element analysis software to establish the numerical model which is based on the test model to carry out the seismic performance simulation. Then, through the improvement measures to get the measures for improved seismic performance.

Shaoyao-Gancao Tang (SGT) is one of the most frequently used compound formulas in the treatment of pain-related diseases in the medical practice of traditional Chinese medicine (TCM). To investigate the anti-inflammatory and antinociceptive effects, as well as to uncover the molecular mechanism of SGT, the rat pain model of arthritis was experimentally induced by single unilateral injection of rats’ left hind paw with Freund’s complete adjuvant (FCA). SGT was orally administered to the rats daily at three doses individually for a period of 16 days post-model induction. Swollen degrees and pain thresholds of the rats in different groups were measured for evaluation of the anti-inflammatory and anti-nociceptive effects of SGT. Furthermore, the mRNA and protein expression levels of transient receptor potential ion channel protein vanilloid receptor 1 (TRPV1) channel as well as its calcium-mediating function in the isolated DRG neurons were further detected to provide indexes for exploration of the molecular mechanisms mediating anti-arthritic activities of SGT. As a result, FCA injection induced significant allodynia, inflammation and edema, accompanied by a significant increase in both expression and calcium-mediating function of the TRPV1 channel. Pharmacologically, oral administration of SGT at a high or middle dose demonstrated a significant relief from the above-mentioned pathological conditions in a dose-dependent manner. Simultaneously the mRNA and protein expressional levels of TRPV1 channel, as well as its calcium-mediating function, were down-regulated greatly. These findings suggest that SGT possesses a significant analgesic and anti-inflammatory effect on arthritis rats; its therapeutic activities might be achieved through reversing the elevated expression and function of TRPV1 channel evoked by FCA.

Identification of the accurate risk factor for CKD remains mandatory to combat the high prevalence of diseases. Growing evidence suggests the association of serum vitamin D with diverse health conditions. However, the relationship between vitamin D, intact parathyroid hormone (PTH), and calcium-phosphate metabolism and development of CKD remains controversial. We conduct this cross-sectional observational study to investigate the association between serum 25 (OH) vitamin D, intact PTH, and calcium and phosphate levels with eGFR and albuminuria, as a surrogate marker of CKD, in a community population. A total of 4080 participants were recruited. The mean age was 58.4 ± 13.3 years and 1480 (36.3%) were men. The mean eGFR was 94.1 ± 26.3 mL/min/1.73 m2. The prevalence of CKD was 19.8%. Serum 25 (OH) vitamin D and log intact PTH levels were inversely correlated with eGFR but positively correlated with log albuminuria. Logistic regression analysis identified the log intact PTH as an independent factor associated with eGFR ≤ 60 mL/min/1.73 m2and proteinuria. This association was consistent when serum intact PTH was analyzed as continuous as well as categorical variables (as hyperparathyroidism). The relationship remains significant using resampling subset analysis with comparable baseline characteristics and adjustment for 25 (OH) vitamin D, calcium, and phosphate levels. This finding warranted further research to clarify the causal relationship of PTH/25 (OH) vitamin D with the risk of CKD in the general population.

We report 1.1 mm number counts revealed with the Atacama Large Millimeter/submillimeter Array (ALMA) in the Subaru/XMM-Newton Deep Survey Field (SXDF). The advent of ALMA enables us to reveal millimeter-wavelength number counts down to the faint end without source confusion. However, previous studies are based on the ensemble of serendipitously-detected sources in fields originally targeting different sources and could be biased due to the clustering of sources around the targets. We derive number counts in the flux range of 0.2-2 mJy by using 23 (>=4sigma) sources detected in a continuous 2.0 arcmin$^2$ area of the SXDF. The number counts are consistent with previous results within errors, suggesting that the counts derived from serendipitously-detected sources are not significantly biased, although there could be field-to-field variation due to the small survey area. By using the best-fit function of the number counts, we find that ~40% of the extragalactic background light at 1.1 mm is resolved at S(1.1mm) > 0.2 mJy., 8 pages, 7 figures, Accepted for publication in PASJ

We have conducted 1.1 mm ALMA observations of a contiguous $105'' \times 50''$ or 1.5 arcmin$^2$ window in the SXDF-UDS-CANDELS. We achieved a 5$��$ sensitivity of 0.28 mJy, providing a flat sensus of dusty star-forming galaxies with $L_{\rm IR} \sim6\times10^{11}$ $L_\odot$ (for $T_{\rm dust}$ =40K) up to $z\sim10$ thanks to the negative K-correction at this wavelength. We detected 5 brightest sources (S/N$>$6) and 18 low-significance sources (5$>$S/N$>$4; these may contain spurious detections, though). One of the 5 brightest ALMA sources ($S_{\rm 1.1mm} = 0.84 \pm 0.09$ mJy) is extremely faint in the WFC3 and VLT/HAWK-I images, demonstrating that a contiguous ALMA imaging survey is able to uncover a faint dust-obscured population that is invisible in deep optical/near-infrared surveys. We found a possible [CII]-line emitter at $z=5.955$ or a low-$z$ CO emitting galaxy within the field, which may allow us to constrain the [CII] and/or the CO luminosity functions across the history of the universe., 4 pages, 2 figures, 1 table, to appear in the proceedings of IAU Symposium 319 "Galaxies at High Redshift and Their Evolution over Cosmic Time", eds. S. Kaviraj & H. Ferguson

We present stacking analyses on our ALMA deep 1.1 mm imaging in the SXDF using 1.6 {\mu}m and 3.6 {\mu}m selected galaxies in the CANDELS WFC3 catalog. We detect a stacked flux of ~0.03-0.05 mJy, corresponding to LIR < 10^11 Lsun and a star formation rate (SFR) of ~ 15 Msun/yr at z = 2. We find that galaxies brighter in the rest-frame near-infrared tend to be also brighter at 1.1 mm, and galaxies fainter than m[3.6um] = 23 do not produce detectable 1.1 mm emission. This suggests a correlation between stellar mass and SFR, but outliers to this correlation are also observed, suggesting strongly boosted star formation or extremely large extinction. We also find tendencies that redder galaxies and galaxies at higher redshifts are brighter at 1.1 mm. Our field contains z ~ 2.5 H-alpha emitters and a bright single-dish source. However, we do not find evidence of bias in our results caused by the bright source. By combining the fluxes of sources detected by ALMA and fluxes of faint sources detected with stacking, we recover a 1.1 mm surface brightness of up to 20.3 +/- 1.2 Jy/deg, comparable to the extragalactic background light measured by COBE. Based on the fractions of optically faint sources in our and previous ALMA studies and the COBE measurements, we find that approximately half of the cosmic star formation may be obscured by dust and missed by deep optical surveys, Much deeper and wider ALMA imaging is therefore needed to better constrain the obscured cosmic star formation history., Comment: accepted for publication in ApJ

Observing galaxies in the radio and submillimeter continuum has the advantage of being unaffected by dust extinction, which is a major drawback of studying galaxy evolution using optical data. Submillimeter single-dish surveys have made tremendous progress in understanding the high-redshift dusty population, but the low angular resolution of single-dish telescopes has also hampered these studies. Our recent JCMT and SMA imaging of high-redshift submillimeter sources revealed z > 4 objects that are radio and optically faint. Such objects cannot be easily identified with the combination of submillimeter single-dish and radio imaging. We also found a large fraction of multiple objects that are blended in single-dish images. Such objects may be early-stage mergers, or dusty starbursts in group environments. Since our work, larger surveys with PdBI and ALMA have been carried out to further address these issues. Additional to submillimeter imaging, future ultradeep EVLA imaging at 20 cm can also detect large samples of ultraluminous star forming galaxies at z ≳ 2. Sensitivities in radio and submillimeter observations have different redshift and dust temperature dependencies. Radio observations are also less affected by confusion. It will be necessary to combine deep surveys in both wavebands in order to achieve a more complete picture of the evolution of high-redshift star forming galaxies.

A comprehensively comparison of the chemical profiles between sun-drying BJ (NBJ) and sulfur-fumigated BJ (SBJ) was conducted by HPLC analysis and the discrepant peaks were identified or tentatively assigned by HPLC-ESI-MSn. A total of 32 chemical components were used for qualitative comparison. Meanwhile, a quantitative comparison of BJwere conducted by HPLC analysis and determining seven compounds from 3 NBJ and 3 SBJ samples dramatic chemical changes were found. After sulfur fumigation, the contents of flavonoids glycosides and phenolic acids were remarkably reduced, but the contents of flavonoids aglycones were significantly increased. Multivariate statistics, including principle component analysis (PCA) and partial least squares discriminate analysis (PLS-DA) were used to investigate the potential damaging effect of sulfur-fumigating process. The PCA score plots showed six samples were clearly classified into the sun-drying and sulfur-fumigating groups. And according to VIP1, the most important chemical markers were apigenin, luteolin and 3,5-dicaffeoylquninic acid which could be used to distinguish NBJ and SBJ samples. Combining the results of qualitative and quantitative analysis, it showed that the sulfur fumigation has a significant effect on BJ.

Measuring star formation rates (SFRs) in high-z galaxies with their rest-frame ultraviolet (UV) continuum can be uncertain because of dust obscuration. Prior studies had used the submillimeter emission at 850 um to determine the intrinsic SFRs of rest-frame UV selected galaxies, but the results suffered from the low sensitivity and poor resolution (~15''). Here, we use ultradeep Very Large Array 1.4 GHz images with ~1''-2'' resolutions to measure the intrinsic SFRs. We perform stacking analyses in the radio images centered on ~3500 Lyman break galaxies (LBGs) at z~4 in the Great Observatories Origins Deep Survey-North and South fields selected with Hubble Space Telescope/Advanced Camera for Surveys data. The stacked radio flux is very low, 0.08+/-0.15 uJy, implying a mean SFR of 6+/-11 M/yr. This is comparable to the uncorrected mean UV SFRs of 5 M/yr, implying that the z~4 LBGs have little dust extinction. The low SFR and dust extinction support the previous results that z~4 LBGs are in general not submillimeter galaxies. We further show that there is no statistically significant excess of dust-hidden star-forming components within ~22 kpc from the LBGs., 6 pages, 3 figures, and 2 tables. Accepted to the Astrophysical Journal (ApJ)

We present sensitive phase-referenced VLBI results on the radio continuum emission from the z=1.87 luminous submillimeter galaxy (SMG) GOODS 850-3. The observations were carried out at 1.4 GHz using the High Sensitivity Array (HSA). Our sensitive tapered VLBI image of GOODS 850-3 at 0.47 x 0.34 arcsec (3.9 x 2.9 kpc) resolution shows a marginally resolved continuum structure with a peak flux density of 148 \pm 38 uJy/beam, and a total flux density of 168 \pm 73 uJy, consistent with previous VLA and MERLIN measurements. The derived intrinsic brightness temperature is > 5 \pm 2 x 10^3 K. The radio continuum position of this galaxy coincides with a bright and extended near-infrared source that nearly disappears in the deep HST optical image, indicating a dusty source of nearly 9 kpc in diameter. No continuum emission is detected at the full VLBI resolution (13.2 x 7.2 mas, 111 x 61 pc), with a 4-sigma point source upper limit of 26 uJy/beam, or an upper limit to the intrinsic brightness temperature of 4.7 x 10^5 K. The extent of the observed continuum source at 1.4 GHz and the derived brightness temperature limits are consistent with the radio emission (and thus presumably the far-infrared emission) being powered by a major starburst in GOODS 850-3, with a star formation rate of ~2500 M_sun/yr. Moreover, the absence of any continuum emission at the full resolution of the VLBI observations indicates the lack of a compact radio AGN source in this z=1.87 SMG., 19 pages, 4 figures, accepted for publication in AJ

A new triterpene glycoside mutongsaponin F (1), together with five known saponins and two known lipids, was isolated from the 70% ethanol extract of the stems of Akebia trifoliata (Thunb.) Koidz. var. australis (Diels) Rehd. Their structures were elucidated on the basis of the spectroscopic analysis and physicochemical properties as 3-beta-[(beta-D-glucopyranosyl-(1-->2)-O-[beta-D-glucopyranosyl-(1-->3)-O-]-alpha-L-arabinopyranosyl)oxy]-30-norolean-12-en-28-oic acid alpha-L-rhamnopyranosyl-(1-->4)-O-beta-D-glucopyranosyl-(1-->6)-O-beta-D-glucopyranosyl ester (1), 3-beta-[(beta-D-glucopyranosyl-(1-->2)-O-[beta-D-glucopyranosyl-(1-->3)-O-]-alpha-L-arabinopyranosyl)oxy]-30-norolean-12-en-28-oic acid (2), leonticin E (3), collinsonidin (4), arjunolic acid 28-O-glucopyranoside (5), asiatic acid 28-O-glucopyranoside (6), soya-cerebroside I (7), and 1-O-alpha-L-galactosyl-(1-->6)-O-beta-D-galactosyl-3-O-hexadecanoyl-glycerol (8), respectively.

We report a highly significant Submillimeter Array (SMA) detection of the prototypical submillimeter source HDF 850.1, which is the brightest submillimeter source in the Hubble Deep Field-North proper. The detection yields an extremely precise position of RA(2000)=12:36:51.99 and Dec(2000)=+62:12:25.83 with a 1-sigma positional uncertainty of 0.17 arcsec. The position is consistent with the location of a millimeter wavelength interferometric detection and with the locations of weak VLA detections at 1.4 and 8.4 GHz, but it is not consistent with any previous optical/near-infrared identifications. The source appears pointlike at the 2 arcsec resolution of the SMA, and the detected flux of 7.8+/-1.0 mJy is consistent with the measured SCUBA fluxes. We tabulate fluxes and limits on HDF 850.1 at other wavelengths. Our redshift estimate for HDF 850.1 based on the radio through mid-infrared measurements is z=4.1. The faintness of the source at optical/near-infrared wavelengths and the high estimated redshift suggest that HDF 850.1 may be an analog of the brighter submillimeter source GOODS 850-5, which is also thought to be at z>4. The fact that a source like HDF 850.1 should have appeared in one of the very first blank-field SCUBA observations ever made suggests that such high-redshift sources are quite common. Thus, we are led to conclude that high-redshift star formation is dominated by giant dusty star-forming galaxies, just as it is at lower redshifts., 5 pages

Phytolacacinoside A (1), a novel triterpenoid saponin, together with the seven known compounds, was isolated from 75% ethanol extract of the root of Phytolacca acinosa Roxb (Phytolaccaceae). Their structures were elucidated on the basis of analysis of spectroscopic data and physicochemical properties as 3-O-beta-[(beta-d-glucopyranosyl-(1 --> 4)-O-beta-D-xylopyranosyl)]-11beta-methoxy-jaligonic acid 30-methyl ester 28-O-beta-D-glucopyranoside (1), 3-O-beta-[(beta-D-glucopyranosyl-(1 --> 4)-O-beta-D-xylopyranosyl)]-jaligonic acid 30-methyl ester 28-O-beta-D-glucopyranoside (2, esculentoside G), 3-O-beta-[(beta-D-glucopyranosyl-(1 --> 4)-O-beta-D-xylopyranosyl)]-jaligonic acid 30-methyl ester (3, phytolaccoside E), 3-O-beta-D-xylopyranosyl-jaligonic acid 30-methyl ester (4, phytolaccoside B), hypaphorine (5), palmitic acid monoglyceride (6), beta-sitosterol (7), and daucosterol (8).

Due to the popularity of location-based services, determining the location of a device at all times has become a subject of great interests. Although many GPS-based applications have been developed and successfully deployed in various fields, their applicabilities are hindered by the obstruction of the objects in the environment. Essentially, as satellite signals cannot penetrate the walls of buildings, the coverage of GPS systems is limited to outdoor environments. To fully exploit the benefit of location-based services, approaches that determine the location of a device in indoor environments need to be established. This study presents a novel location determination mechanism that uses an indoor WLAN and back-propagation neural network (BPN). A museum is taken as the context of the example indoor environment. Location determination is achieved using the combined strengths of 802.11b wireless access signals. With a significant number of access points (APs) installed in the museum, hand-held devices can sense the strengths of the signals from all APs to which the devices can connect. Using a back-propagation network, device locations can be estimated with sufficient accuracy. A novel adaptive algorithm is implemented for enhancing the accuracy of the estimation.

The submillimeter (submm) extragalactic background light (EBL) traces the integrated star formation history throughout the cosmic time. Deep blank-field 850 μm and 1.4 GHz surveys and optical follow-up have been only able to determine the redshift of ∼20% of the submm EBL. The majority (80%) of the submm EBL is still below the confusion and sensitivity limits of current submm and radio instruments. We break through these limits with stacking analyses on our deep 850 μm image in the GOODS-N and find that the submm EBL mostly comes from galaxies at redshifts around 1.0. This redshift is much lower than the redshift of z=2–3 previously implied from radio identified submm sources. This result significantly decreases the number of high redshift galaxies that may be seen by ALMA.

Ethnopharmacological relevance Gastrodia elata Blume ( Orchidaceae ) is commonly called Tian ma in Chinese and mainly distributed in the mountainous areas of eastern Asia, such as China, Korea, Japan and India. It is an extensively used traditional Chinese herbal medicine in the clinical practice of traditional Chinese medicine, to treat headache, migraine, dizziness, epilepsy, infantile convulsion, tetany and so on. The present paper reviews the advancements in investigation of botany and ethnopharmacology, phytochemistry, pharmacology, toxicology and quality control of Gastrodia elata Blume. Finally, the possible tendency and perspective for future investigation of this plant are also put forward. Materials and methods The information on Gastrodia elata Blume was collected via piles of resources including classic books about Chinese herbal medicine, and scientific databases including Pubmed, Google Scholar, ACS, Web of science, ScienceDirect databases, CNKI and others. Plant taxonomy was validated by the databases “The Plant List”, and “Mansfeld’s Encyclopedia”. Results Over 81 compounds from this plant have been isolated and identified, phenolics and polysaccharides are generally considered as the characteristic and active constituents of Gastrodia elata Blume. Its active compounds possess wide-reaching biological activities, including sedative, hypnotic, antiepileptic, anticonvulsive, antianxietic, antidepressant, neuroprotective, antipsychotic, anti-vertigo, circulatory system modulating, anti-inflammationary, analgesic, antioxidative, memory-improving and antiaging, antivirus and antitumor effects. Conclusion Despite the publication of various papers on Gastrodia elata Blume, there is still, however, the need for definitive research and clarification of other bioactive compounds using bioactivity-guided isolation strategies, and the possible mechanism of action as well as potential synergistic or antagonistic effects of multi-component mixtures derived from Gastrodia elata Blume need to be evaluated. It is also necessary and important to do more quality control and toxicological study on human subjects in order to maintain its efficacy stable in the body and validate its safety in clinical uses. In addition, more investigations on other parts of this plant beyond the tubers are needed. Further studies on Gastrodia elata Blume will lead to the development of new drugs and therapeutics for various diseases, and how to utilize it better should be paid more attention to.

Ground-based observations at terahertz (THz) frequencies are a newly explorable area of astronomy for the next ten years. We discuss science cases for a first-generation 10-m class THz telescope, focusing on the Greenland Telescope as an example of such a facility. We propose science cases and provide quantitative estimates for each case. The largest advantage of ground-based THz telescopes is their higher angular resolution (~ 4 arcsec for a 10-m dish), as compared to space or airborne THz telescopes. Thus, high-resolution mapping is an important scientific argument. In particular, we can isolate zones of interest for Galactic and extragalactic star-forming regions. The THz windows are suitable for observations of high-excitation CO lines and [N II] 205 um lines, which are scientifically relevant tracers of star formation and stellar feedback. Those lines are the brightest lines in the THz windows, so that they are suitable for the initiation of ground-based THz observations. THz polarization of star-forming regions can also be explored since it traces the dust population contributing to the THz spectral peak. For survey-type observations, we focus on ``sub-THz'' extragalactic surveys, whose uniqueness is to detect galaxies at redshifts z ~ 1--2, where the dust emission per comoving volume is the largest in the history of the Universe. Finally we explore possibilities of flexible time scheduling, which enables us to monitor active galactic nuclei, and to target gamma-ray burst afterglows. For these objects, THz and submillimeter wavelength ranges have not yet been explored., 39 pages, 17 figures, accepted for publication in PASJ (as a review paper)

We present first results from the SXDF-ALMA 1.5 arcmin^2 deep survey at 1.1 mm using Atacama Large Millimeter Array (ALMA). The map reaches a 1sigma depth of 55 uJy/beam and covers 12 Halpha-selected star-forming galaxies at z = 2.19 or z=2.53. We have detected continuum emission from three of our Halpha-selected sample, including one compact star-forming galaxy with high stellar surface density, NB2315-07. They are all red in the rest-frame optical and have stellar masses of log (M*/Msun)>10.9 whereas the other blue, main-sequence galaxies with log(M*/Msun)=10.0-10.8 are exceedingly faint, 6 pages, 4 figures, 1 table, accepted for publication in ApJL

We use new deep near-infrared (NIR) and mid-infrared (MIR) observations to analyze the 850$~��$m image of the GOODS HDF-N region. We show that much of the submillimeter background at this wavelength is picked out by sources with $H(AB)$ or 3.6um (AB), 14 pages, 15 figures. Accepted by The Astrophysical Journal for v647n 1 issue, August 2006. Minor changes in response to the referee's report, plus a new comparison figure of the star formation history measured in the FIR with that measured in the UV. We plot d(rho)/dt x cosmic time vs. cosmic time, which has the advantage of illustrating more directly how many stars are formed at a given time

The Hubble Deep Field-North (HDF-N) is one of the best studied extragalactic fields, and ultra-deep optical, radio, X-ray, and mid-infrared wide-field images are available for this area. Here we present an 850 um survey around the HDF-N, covering most of the area imaged by the Advanced Camera for Surveys as a part of the Great Observatories Origins Deep Survey. Our map has 0.4-4 mJy sensitivities (1 sigma) over an area ~110 arcmin^2 and there are 45 sources detected at >3 sigma. After correcting the effects of noise, confusion, incompleteness, and the Eddington bias using Monte Carlo simulations, we find that the detected 850 $\mu$m sources with fluxes greater than 2 mJy have a surface density of 3200^+1900_-1000 deg^-2 and account for about 24% to 34% of the far-infrared extragalactic background light. Using the deep radio interferometric image and the deep X-ray image, we are able to accurately locate ~60% of the bright submillimeter (submm) sources. In addition, by assuming the Arp 220 spectral energy distribution in the submm and radio, we estimate millimetric redshifts for the radio detected submm sources, and redshift lower limits for the ones not detected in the radio. Using the millimetric redshifts of the radio identified sources and spectroscopic and optical photometric redshifts for galaxies around the submm positions, we find a median redshift of 2.0 for 11 possibly identified sources, or a lower limit of 2.4 for the median redshift of our 4 sigma sample.

The SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES) is a three-year JCMT Large Program aiming at reaching the 450 $\mu$m confusion limit in the COSMOS-CANDELS region, to study a representative sample of the high-redshift far-infrared galaxy population that gives rise to the bulk of the far-infrared background. We present the first-year data from STUDIES. We have reached a 450 $\mu$m noise level of 0.91~mJy for point sources at the map center, covered an area of 151 arcmin$^2$, and detected 98 and 141 sources at 4.0 and 3.5 $\sigma$, respectively. Our derived counts are best constrained in the 3.5-25 mJy regime using directly detected sources. Below the detection limits, our fluctuation analysis further constrains the slope of the counts down to 1 mJy. The resulting counts at 1-25 mJy are consistent with a power law having a slope of $-2.59$ ($\pm0.10$ for 3.5-25 mJy, and $^{+0.4}_{-0.7}$ for 1-3.5 mJy). There is no evidence of a faint-end termination or turn-over of the counts in this flux density range. Our counts are also consistent with previous SCUBA-2 blank-field and lensing cluster surveys. The integrated surface brightness from our counts down to 1 mJy is $90.0\pm17.2$ Jy deg$^{-2}$, which can account for up to $83^{+15}_{-16}\%$ of the COBE 450 $\mu$m background. We show that Herschel counts at 350 and 500 $\mu$m are significantly higher than our 450 $\mu$m counts, likely caused by its large beam and source clustering. High-angular resolution instruments like SCUBA-2 at 450 $\mu$m are therefore highly beneficial for measuring the luminosity and spatial density of high-redshift dusty galaxies., Comment: ApJ accepted. revised version uploaded