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1. Assessment of Prostate Volume and Prostate-specific Antigen Density With the Segmentation Method on Magnetic Resonance Imaging

Author: LIN, YEN-TING, HUNG, SIU-WAN, CHIU, KUN-YUAN, CHAI, JYH-WEN, and LIN, JIN-CHING
Subjects: Pharmacology, Cancer Research, General Biochemistry, Genetics and Molecular Biology, Research Article
Abstract: Background/Aim: This study aimed to compare the prostate volume (PV) and prostate-specific antigen density (PSAD) obtained using the ellipsoid volume formula or segmentation methods on magnetic resonance imaging (MRI) and further predict prostate cancer (PCa). Patients and Methods: Retrospectively, the enrolled patients underwent prostate MRI and had PSA levels between 4 and 10 ng/ml. The PV was measured with both the ellipsoid volume formula (PVe) and the segmentation method (PVs). The transitional zone volume (TZV) was measured with the segmentation method. The PSADe, PSADs, and PSAD_TZV were calculated. Bland-Altman plots were used to compare the agreements. ROC curve analysis was used to compare the diagnostic accuracies to predict PCa. The results were also compared between the PCa and the no-PCa groups, and among tumors with different locations and different Gleason scores (GS). Results: Seventy-six of the 117 enrolled patients were classified into the PCa group. There were high agreements between PVs and PVe as well as between PSADs and PSADe, while several outliers were mainly due to post-transurethral resection of the prostate changes and irregular hyperplastic nodules. The diagnostic accuracy of PSADe (AUC: 0.732) was slightly higher than that of PSADs (AUC: 0.729) and PSAD_TZV (AUC: 0.715). The PSADe and PSADs were not different among different tumor locations but were higher in GS ≥7 lesions (both p=0.006). Conclusion: The segmentation method can be an alternative method to measure PV and calculate PSAD before prostate biopsy, particularly in post-transurethral resection of the prostate patients or those with irregular hyperplastic nodules.
Published: 2023
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2. Improving Estimation of the Koopman Operator with Kolmogorov-Smirnov Indicator Functions

Author: Ngo, Van A., Lin, Yen Ting, and Perez, Danny
Subjects: FOS: Computer and information sciences, Statistics - Machine Learning, Biological Physics (physics.bio-ph), Physics - Data Analysis, Statistics and Probability, FOS: Physical sciences, Machine Learning (stat.ML), Physics - Biological Physics, Computational Physics (physics.comp-ph), Physics - Computational Physics, Data Analysis, Statistics and Probability (physics.data-an)
Abstract: It has become common to perform kinetic analysis using approximate Koopman operators that transforms high-dimensional time series of observables into ranked dynamical modes. Key to a practical success of the approach is the identification of a set of observables which form a good basis in which to expand the slow relaxation modes. Good observables are, however, difficult to identify {\em a priori} and sub-optimal choices can lead to significant underestimations of characteristic timescales. Leveraging the representation of slow dynamics in terms of Hidden Markov Model (HMM), we propose a simple and computationally efficient clustering procedure to infer surrogate observables that form a good basis for slow modes. We apply the approach to an analytically solvable model system, as well as on three protein systems of different complexities. We consistently demonstrate that the inferred indicator functions can significantly improve the estimation of the leading eigenvalues of the Koopman operators and correctly identify key states and transition timescales of stochastic systems, even when good observables are not known {\em a priori}., Comment: 28 pages, 6 figures
Published: 2023
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3. AN EMPIRICAL STUDY ON PARENTS' CHOICES APPLY ON ALTERNATIVE EDUCATION: A CASE STUDY OF T SCHOOL IN BEIJING

Author: Lin Yen-Ting
Subjects: Empirical research, Beijing, Mathematics education, Sociology, Alternative education
Published: 2020
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4. SalesBot: Transitioning from Chit-Chat to Task-Oriented Dialogues

Author: Chiu, Ssu, Li, Maolin, Lin, Yen-Ting, and Chen, Yun-Nung
Subjects: FOS: Computer and information sciences, Artificial Intelligence (cs.AI), Computer Science - Computation and Language, Computer Science - Artificial Intelligence, Computation and Language (cs.CL)
Abstract: Dialogue systems are usually categorized into two types, open-domain and task-oriented. The first one focuses on chatting with users and making them engage in the conversations, where selecting a proper topic to fit the dialogue context is essential for a successful dialogue. The other one focuses on a specific task instead of casual talks, e.g., finding a movie on Friday night, or playing a song. These two directions have been studied separately due to their different purposes. However, how smoothly transitioning from social chatting to task-oriented dialogues is important for triggering business opportunities, and there is no public data focusing on such scenarios. Hence, this paper focuses on investigating the conversations starting from open-domain social chatting and then gradually transitioning to task-oriented purposes, and releases a large-scale dataset with detailed annotations for encouraging this research direction. To achieve this goal, this paper proposes a framework to automatically generate many dialogues without human involvement, in which any powerful open-domain dialogue generation model can be easily leveraged. The human evaluation shows that our generated dialogue data has a natural flow at a reasonable quality, showing that our released data has a great potential of guiding future research directions and commercial activities. Furthermore, the released models allow researchers to automatically generate unlimited dialogues in the target scenarios, which can greatly benefit semi-supervised and unsupervised approaches., ACL 2022
Published: 2022
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5. A systematic search for proto-cluster cores at a transition epoch of star formation activity

Author: Ando, Makoto, Shimasaku, Kazuhiro, Momose, Rieko, Shimakawa, Rhythm, Sawicki, Marcin, Ito, Kei, and Lin, Yen-Ting
Subjects: Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: At$z>2$, galaxies in proto-clusters (PCs) are actively star forming, while matured clusters at $z are dominated by quenched galaxies, suggesting that \(z\sim1.5$ is a transition epoch of (proto-)clusters from star forming phase into quenching phase. To investigate galaxy evolution in this transition epoch, we search for PC cores at $z\sim1.5$. Here, a "core" is defined as the most massive halo in a given PC, where environmental effects are likely to work most effectively. Using a photo-z catalog of large and deep optical survey data with Subaru Hyper-Suprime Cam, we search for PC cores in a very wide field that reaches $\sim22 \, \mathrm{deg}^{2}$. Regarding galaxies more massive than $\sim2 \times 10^{11}\, M_{\odot}$ as the central galaxies of PC cores, we detect more than 1000 core candidates. Then, we estimate their average halo mass by clustering analysis and find it to be $\sim3 \times 10^{13}\, M_{\odot}$. From a comparison with the Illustris TNG simulation, we confirm that these massive halos at$z\sim1.5$ are progenitors of present-day clusters comparable to or more massive than Fornax-type clusters. Classifying our galaxy sample into red and blue galaxies, we calculate the red fraction of the member galaxies of our PC core candidates. Although red and blue centrals have similar halo masses, only the red fraction around red centrals shows an excess compared to the field, while that around blue centrals shows no excess, suggesting a conformity effect. We discuss galaxy quenching in PC cores at $z\sim1.5$.
Published: 2021
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6. SITELLE H�� Imaging Spectroscopy of z~0.25 Clusters: Emission Line Galaxy Detection and Ionized Gas Offset in Abell 2390 & Abell 2465

Author: Liu, Qing, Yee, Howard, Drissen, Laurent, Sivanandam, Suresh, Pintos-Castro, Irene, Alcorn, Leo Y., Hsieh, Bau-Ching, Lin, Lihwai, Lin, Yen-Ting, Muzzin, Adam, Noble, Allison, and Old, Lyndsay
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Environmental effects are crucial to the understanding of the evolution of galaxies in dense environments, such as galaxy clusters. Using the large field-of-view of SITELLE, the unique imaging fourier transform spectrograph at CFHT, we are able to obtain 2D spectral information for a large and complete sample of cluster galaxies out to the infall region. We describe a pipeline developed to identify emission line galaxies (ELGs) from the datacube using cross-correlation techniques. We present results based on the spatial offsets between the emission-line regions and stellar continua in ELGs from two z$\sim$0.25 galaxy clusters, Abell 2390 and Abell 2465. We find a preference in the offsets being pointed away from the cluster center. Combining the two clusters, there is a 3$��$ excess for high-velocity galaxies within the virial radius having the offsets to be pointed away from the cluster center. Assuming the offset being a proxy for the velocity vector of a galaxy, as expected from ram pressure stripping, this excess indicates that ram pressure stripping occurs most effectively during the first passage of an infalling galaxy, leading to the quenching of its star formation. We also find that, outside the virial region, the continuum-normalized H$��$ line flux for infalling galaxies with large offsets are on average lower than those with small or no measurable offset, further supporting ram pressure as a dominant quenching mechanism during the initial infall stages., 25 pages, 18 figures, accepted for publication in ApJ
Published: 2021
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7. What needles do sparse neural networks find in nonlinear haystacks

Author: Sardy, Sylvain, Hengartner, Nicolas W, Bonenko, Nikolai, and Lin, Yen Ting
Subjects: FOS: Computer and information sciences, Computer Science - Machine Learning, Statistics - Machine Learning, Physics - Data Analysis, Statistics and Probability, FOS: Physical sciences, Machine Learning (stat.ML), Data Analysis, Statistics and Probability (physics.data-an), Machine Learning (cs.LG)
Abstract: Using a sparsity inducing penalty in artificial neural networks (ANNs) avoids over-fitting, especially in situations where noise is high and the training set is small in comparison to the number of features. For linear models, such an approach provably also recovers the important features with high probability in regimes for a well-chosen penalty parameter. The typical way of setting the penalty parameter is by splitting the data set and performing the cross-validation, which is (1) computationally expensive and (2) not desirable when the data set is already small to be further split (for example, whole-genome sequence data). In this study, we establish the theoretical foundation to select the penalty parameter without cross-validation based on bounding with a high probability the infinite norm of the gradient of the loss function at zero under the zero-feature assumption. Our approach is a generalization of the universal threshold of Donoho and Johnstone (1994) to nonlinear ANN learning. We perform a set of comprehensive Monte Carlo simulations on a simple model, and the numerical results show the effectiveness of the proposed approach., Comment: 8 pages, 2 figures
Published: 2020
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8. A Power-Efficient Binary-Weight Spiking Neural Network Architecture for Real-Time Object Classification

Author: Tan, Pai-Yu, Chuang, Po-Yao, Lin, Yen-Ting, Wu, Cheng-Wen, and Lu, Juin-Ming
Subjects: Signal Processing (eess.SP), FOS: Computer and information sciences, Computer Vision and Pattern Recognition (cs.CV), Hardware Architecture (cs.AR), Computer Science - Computer Vision and Pattern Recognition, FOS: Electrical engineering, electronic engineering, information engineering, Computer Science - Neural and Evolutionary Computing, Neural and Evolutionary Computing (cs.NE), Electrical Engineering and Systems Science - Signal Processing, Computer Science - Hardware Architecture
Abstract: Neural network hardware is considered an essential part of future edge devices. In this paper, we propose a binary-weight spiking neural network (BW-SNN) hardware architecture for low-power real-time object classification on edge platforms. This design stores a full neural network on-chip, and hence requires no off-chip bandwidth. The proposed systolic array maximizes data reuse for a typical convolutional layer. A 5-layer convolutional BW-SNN hardware is implemented in 90nm CMOS. Compared with state-of-the-art designs, the area cost and energy per classification are reduced by 7$\times$ and 23$\times$, respectively, while also achieving a higher accuracy on the MNIST benchmark. This is also a pioneering SNN hardware architecture that supports advanced CNN architectures.
Published: 2020
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9. Angular clustering and host halo properties of [OII] emitters at $z >1$ in the Subaru HSC survey

Author: Okumura, Teppei, Hayashi, Masao, Chiu, I-Non, Lin, Yen-Ting, Osato, Ken, Hsieh, Bau-Ching, and Lin, Sheng-Chieh
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences
Abstract: We study the angular correlation function of star-forming galaxies and properties of their host dark matter halos at z>1 using the Hyper-Suprime Cam (HSC) SSP survey. We use [OII] emitters identified using two narrow-band (NB) filters, NB816 and NB921, in the Deep/UltraDeep layers, which respectively cover large angular areas of 16.3 deg^2 and 16.9 deg^2. Our sample contains 8302 and 9578 [OII] emitters at z=1.19 (NB816) and z=1.47 (NB921), respectively. We detect a strong clustering signal over a wide angular range, 0.001 < ��< 1 [deg], with the bias $b=1.61^{+0.13}_{-0.11}$ (z=1.19) and $b=2.09^{+0.17}_{-0.15}$ (z=1.47). We also find a clear deviation of the correlation from a simple power-law form. To interpret the measured clustering signal, we adopt a halo occupation distribution (HOD) model that is constructed to explain the spatial distribution of galaxies selected by a star formation rate. The observed correlation function and number density are simultaneously explained by the best-fitting HOD model. From the constrained HOD model, the average mass of halos hosting the [OII] emitters is derived to be $\log{M_{eff}/(h^{-1}M_\odot)}=12.70^{+0.09}_{-0.07}$ and $12.61^{+0.09}_{-0.05}$ at z=1.19 and 1.47, respectively, which will become halos with the present-day mass, $M\sim 1.5 \times 10^{13}h^{-1}M_\odot$. The satellite fraction of the [OII] emitter sample is found to be $f_{sat}\sim 0.15$. All these values are consistent with the previous studies of similar samples, but we obtain tighter constraints even in a larger parameter space due to the larger sample size from the HSC. The results obtained for host halos of [OII] emitters in this paper enable the construction of mock galaxy catalogs and the systematic forecast study of cosmological constraints from upcoming emission line galaxy surveys such as the Subaru PFS survey., 21 pages, 13 figures, 5 tables, accepted to PASJ
Published: 2020
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10. A 16 deg$^2$ survey of emission-line galaxies at z<1.6 from HSC-SSP PDR2 and CHORUS

Author: Hayashi, Masao, Shimakawa, Rhythm, Tanaka, Masayuki, Onodera, Masato, Koyama, Yusei, Inoue, Akio K., Komiyama, Yutaka, Lee, Chien-Hsiu, Lin, Yen-Ting, and Yabe, Kiyoto
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences
Abstract: We have conducted a comprehensive survey of emission-line galaxies at $z\lesssim1.6$ based on narrowband (NB) imaging data taken with Hyper Suprime-Cam (HSC) on the Subaru telescope. In this paper, we update the catalogs of H$��$, [OIII], and [OII] emission-line galaxies using the data from the second Public Data Release (PDR2) of Subaru Strategic Program (SSP) of HSC and Cosmic HydrOgen Reionization Unveiled with Subaru (CHORUS) survey along with the spectroscopic redshifts for 2,019 emission-line galaxies selected with the PDR1 data. The wider effective coverage of NB816 and NB921, 16.3 deg$^2$ and 16.9 deg$^2$ respectively, are available in the Deep and UltraDeep layers of HSC-SSP from the PDR2. The CHORUS survey provides us with data with additional three NBs (NB527, NB718, and NB973) in the COSMOS field in the UltraDeep layer (1.37 deg$^2$). The five NB datasets allow us to investigate the star-forming galaxies presenting emission-lines at 14 specific redshifts ranging from $z\sim1.6$ down to $z\sim0.05$. We revisit the distribution of large-scale structures and luminosity functions (LFs) for the emission-line galaxies with the large samples of 75,377 emission-line galaxies selected. The redshift revolution of LFs shows that the star formation rate densities (SFRDs) decreases monotonically from $z\sim1.6$, which is consistent with the cosmic SFRD ever known. Our samples of emission-line galaxies covering a sufficiently large survey volume are useful to investigate the evolution of star-forming galaxies since the cosmic noon in a wide range of environments including galaxy clusters, filaments, and voids., 32 pages, 23 figures, 6 tables, accepted for publication in PASJ. The catalog of emission-line galaxies from HSC-SSP PDR2 data will be available soon at https://hsc-release.mtk.nao.ac.jp/, and the catalog from CHORUS data will be available after the CHORUS data are publicly released
Published: 2020
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11. SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES) IV: Spatial clustering and halo masses of 450-$��$m-selected sub-millimeter galaxies

Author: Lim, Chen-Fatt, Chen, Chian-Chou, Smail, Ian, Wang, Wei-Hao, Tee, Wei-Leong, Lin, Yen-Ting, Scott, Douglas, Toba, Yoshiki, Chang, Yu-Yen, Ao, YiPing, Babul, Arif, Bunker, Andy, Chapman, Scott C., Clements, David L, Conselice, Christopher J., Gao, Yu, Greve, Thomas R., Ho, Luis C., Hong, Sungwook E., Hwang, Ho Seong, Koprowski, Maciej, Micha��owski, Micha�� J., Shim, Hyunjin, Shu, Xinwen, and Simpson, James M.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences
Abstract: We analyze an extremely deep 450-$��$m image ($1��=0.56$\,mJy\,beam$^{-1}$) of a $\simeq 300$\,arcmin$^{2}$ area in the CANDELS/COSMOS field as part of the SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES). We select a robust (signal-to-noise ratio $\geqslant 4$) and flux-limited ($\geqslant 4$\,mJy) sample of 164 sub-millimeter galaxies (SMGs) at 450-$��$m that have $K$-band counterparts in the COSMOS2015 catalog identified from radio or mid-infrared imaging. Utilizing this SMG sample and the 4705 $K$-band-selected non-SMGs that reside within the noise level $\leqslant 1$\,mJy\,beam$^{-1}$ region of the 450-$��$m image as a training set, we develop a machine-learning classifier using $K$-band magnitude and color-color pairs based on the thirteen-band photometry available in this field. We apply the trained machine-learning classifier to the wider COSMOS field (1.6\,deg$^{2}$) using the same COSMOS2015 catalog and identify a sample of 6182 450-$��$m SMG candidates with similar colors. The number density, radio and/or mid-infrared detection rates, redshift and stellar mass distributions, and the stacked 450-$��$m fluxes of these SMG candidates, from the S2COSMOS observations of the wide field, agree with the measurements made in the much smaller CANDELS field, supporting the effectiveness of the classifier. Using this 450-$��$m SMG candidate sample, we measure the two-point autocorrelation functions from $z=3$ down to $z=0.5$. We find that the 450-$��$m SMG candidates reside in halos with masses of $\simeq (2.0\pm0.5) \times10^{13}\,h^{-1}\,\rm M_{\odot}$ across this redshift range. We do not find evidence of downsizing that has been suggested by other recent observational studies., ApJ accepted
Published: 2020
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12. Spatially resolving properties of galaxies across cosmic time with piXedfit

Author: Abdurro'uf, Lin, Yen-Ting, and Akiyama, Masayuki
Subjects: Astrophysics::Instrumentation and Methods for Astrophysics, galaxy evolution, Astrophysics::Cosmology and Extragalactic Astrophysics, Bayesian statistical inference, galaxy formation, galaxy physical properties, Astrophysics::Galaxy Astrophysics
Abstract: Currently, most photometric studies of galaxies have only been done by treating a galaxy as a single point object or modeling them with a few axisymmetric components. The advent of IFU surveys has revolutionized the way we study galaxies. Despite its powerful capabilities, wide-area IFU surveys are only limited to local galaxies. The latest development in the spectral energy distribution (SED) fitting method makes it possible to implement the method on a pixel-to-pixel basis. piXedfit, pixelized SED fitting, is a python package that provides tools for obtaining spatially resolved stellar population properties of galaxies from multi-band imaging data. This package will be an essential tool for studying the stellar population properties of galaxies across a wide redshift range in the era of big data in photometry (from JWST, WFIRST, LSST, and Euclid).
Published: 2019
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13. A 290MV Ultra-Low Voltage One-Port SRAM Compiler Design Using a 12T Write Contention and Read Upset Free Bit-Cell in 7NM FinFET Technology

Author: H. J. Liao, Lin Yen-Ting, Mahmut E. Sinangil, and Jonathan Chang
Subjects: Bit cell, business.industry, Computer science, Hardware_PERFORMANCEANDRELIABILITY, computer.software_genre, Multiplexing, Upset, Compiler construction, Static random-access memory, Compiler, business, Low voltage, computer, Testability, Computer hardware
Abstract: In this work, we present an ultra-low voltage SRAM compiler targeting small to medium array sizes to provide a smaller area solution compared to conventional 6T -based SRAMs. A 12T write contention and read upset free bit-cell is used in the design. Array architecture employs a read-modify-write scheme to support bit-write masking and column multiplexing. Built-in-self-test (BIST) and synchronous write-through (SWT) options are also supported to provide testability features while power management (PM) option is included to provide low-leakage sleep and shut-down modes. Proposed design is fabricated in 7nm FinFET technology and achieves lowest reported Vmin of 290mV in this technology.
Published: 2018
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14. Accelerated Bayesian inference of gene expression models from snapshots of single-cell transcripts

Author: Lin, Yen Ting and Buchler, Nicolas E.
Subjects: Computer science, Numerical analysis, Model selection, Monte Carlo method, Posterior probability, Bayesian probability, Markov process, FOS: Physical sciences, Poisson distribution, Bayesian inference, Quantitative Biology - Quantitative Methods, symbols.namesake, Bayesian information criterion, Biological Physics (physics.bio-ph), Physics - Data Analysis, Statistics and Probability, FOS: Biological sciences, symbols, Statistical inference, Kinetic Monte Carlo, Physics - Biological Physics, Uncertainty quantification, Akaike information criterion, Algorithm, Quantitative Methods (q-bio.QM), Data Analysis, Statistics and Probability (physics.data-an)
Abstract: Understanding how stochastic gene expression is regulated in biological systems using snapshots of single-cell transcripts requires state-of-the-art methods of computational analysis and statistical inference. A Bayesian approach to statistical inference is the most complete method for model selection and uncertainty quantification of kinetic parameters from single-cell data. This approach is impractical because current numerical algorithms are too slow to handle typical models of gene expression. To solve this problem, we first show that time-dependent mRNA distributions of discrete-state models of gene expression are dynamic Poisson mixtures, whose mixing kernels are characterized by a piece-wise deterministic Markov process. We combined this analytical result with a kinetic Monte Carlo algorithm to create a hybrid numerical method that accelerates the calculation of time-dependent mRNA distributions by 1000-fold compared to current methods. We then integrated the hybrid algorithm into an existing Monte Carlo sampler to estimate the Bayesian posterior distribution of many different, competing models in a reasonable amount of time. We validated our method of accelerated Bayesian inference on several synthetic data sets. Our results show that kinetic parameters can be reasonably constrained for modestly sampled data sets, if the model is known \textit{a priori}. If the model is unknown,the Bayesian evidence can be used to rigorously quantify the likelihood of a model relative to other models from the data. We demonstrate that Bayesian evidence selects the true model and outperforms approximate metrics, e.g., Bayesian Information Criterion (BIC) or Akaike Information Criterion (AIC), often used for model selection., Comment: 13 pages, 5 figures, 1 Algorithm
Published: 2018
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15. The Massive and Distant Clusters of WISE Survey. I: Survey Overview and a Catalog of >2000 Galaxy Clusters at z~1

Author: Gonzalez, Anthony H., Gettings, Daniel P., Brodwin, Mark, Eisenhardt, Peter R. M., Stanford, S. Adam, Wylezalek, Dominika, Decker, Bandon, Marrone, Daniel P., Moravec, Emily, O'Donnell, Christine, Stalder, Brian, Stern, Daniel, Abdulla, Zubair, Brown, Gillen, Carlstrom, John, Chambers, Kenneth C., Hayden, Brian, Lin, Yen-Ting, Magnier, Eugene, Masci, Frank, Mantz, Adam B., McDonald, Michael, Mo, Wenli, Perlmutter, Saul, Wright, Edward L., and Zeimann, Gregory R.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present the Massive and Distant Clusters of WISE Survey (MaDCoWS), a search for galaxy clusters at 0.7-30 degrees) and the remainder of the southern extragalactic sky at Dec, 26 pages, 17 figures, submitted to The Astrophysical Journal Supplement Series. Machine readable versions of tables 3-6 are included with the source files in the arXiv submission
Published: 2018
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16. Exact and efficient hybrid Monte Carlo algorithm for accelerated Bayesian inference of gene expression models from snapshots of single-cell transcripts

Author: Lin, Yen Ting and Buchler, Nicolas E.
Subjects: Models, Genetic, 010304 chemical physics, Computer science, Model selection, Monte Carlo method, Bayesian probability, Gene Expression, General Physics and Astronomy, Bayes Theorem, 010402 general chemistry, Bayesian inference, 01 natural sciences, 0104 chemical sciences, Hybrid Monte Carlo, ARTICLES, Theoretical Methods and Algorithms, 0103 physical sciences, Statistical inference, Kinetic Monte Carlo, Single-Cell Analysis, Physical and Theoretical Chemistry, Uncertainty quantification, Monte Carlo Method, Algorithm, Algorithms
Abstract: Single cells exhibit a significant amount of variability in transcript levels, which arises from slow, stochastic transitions between gene expression states. Elucidating the nature of these states and understanding how transition rates are affected by different regulatory mechanisms require state-of-the-art methods to infer underlying models of gene expression from single cell data. A Bayesian approach to statistical inference is the most suitable method for model selection and uncertainty quantification of kinetic parameters using small data sets. However, this approach is impractical because current algorithms are too slow to handle typical models of gene expression. To solve this problem, we first show that time-dependent mRNA distributions of discrete-state models of gene expression are dynamic Poisson mixtures, whose mixing kernels are characterized by a piecewise deterministic Markov process. We combined this analytical result with a kinetic Monte Carlo algorithm to create a hybrid numerical method that accelerates the calculation of time-dependent mRNA distributions by 1000-fold compared to current methods. We then integrated the hybrid algorithm into an existing Monte Carlo sampler to estimate the Bayesian posterior distribution of many different, competing models in a reasonable amount of time. We demonstrate that kinetic parameters can be reasonably constrained for modestly sampled data sets if the model is known a priori. If there are many competing models, Bayesian evidence can rigorously quantify the likelihood of a model relative to other models from the data. We demonstrate that Bayesian evidence selects the true model and outperforms approximate metrics typically used for model selection.
Published: 2019
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17. Individual Stellar Halos of Massive Galaxies Measured to 100 kpc at $0.3

Author: Huang, Song, Leauthaud, Alexie, Greene, Jenny, Bundy, Kevin, Lin, Yen-Ting, Tanaka, Masayuki, Miyazaki, Satoshi, and Komiyama, Yutaka
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Massive galaxies display extended light profiles that can reach several hundreds of kilo parsecs. These stellar halos provide a fossil record of galaxy assembly histories. Using data that is both wide (~100 square degree) and deep (i>28.5 mag/arcsec^2 in i-band), we present a systematic study of the stellar halos of a sample of more than 3000 galaxies at 0.3 < z < 0.5 with $\log M_{\star}/M_{\odot} > 11.4$. Our study is based on high-quality (0.6 arcsec seeing) imaging data from the Hyper Suprime-Cam (HSC) Subaru Strategic Program (SSP), which enables us to individually estimate surface mass density profiles to 100 kpc without stacking. As in previous work, we find that more massive galaxies exhibit more extended outer profiles. When this extended light is not properly accounted for as a result of shallow imaging or inadequate profile modeling, the derived stellar mass function can be significantly underestimated at the highest masses. Across our sample, the ellipticity of outer light profiles increases substantially as we probe larger radii. We show for the first time that these ellipticity gradients steepen dramatically as a function of galaxy mass, but we detect no mass-dependence in outer color gradients. Our results support the two-phase formation scenario for massive galaxies in which outer envelopes are built up at late times from a series of merging events. We provide surface mass surface mass density profiles in a convenient tabulated format to facilitate comparisons with predictions from numerical simulations of galaxy formation., Submitted to MNRAS; 23 pages, 8 figures, 2 appendix; Data will be made available here: http://massivegalaxies.com/ once the paper is published
Published: 2017
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18. A 16 deg$^2$ survey of emission-line galaxies at z<1.5 in HSC-SSP PDR1

Author: Hayashi, Masao, Tanaka, Masayuki, Shimakawa, Rhythm, Furusawa, Hisanori, Momose, Rieko, Koyama, Yusei, Silverman, John D., Kodama, Tadayuki, Komiyama, Yutaka, Leauthaud, Alexie, Lin, Yen-Ting, Miyazaki, Satoshi, Nagao, Tohru, Nishizawa, Atsushi J., Ouchi, Masami, Shibuya, Takatoshi, Tadaki, Ken-ichi, and Yabe, Kiyoto
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences
Abstract: We present initial results from the Subaru Strategic Program (SSP) with Hyper Suprime-Cam (HSC) on a comprehensive survey of emission-line galaxies at z5\times10^5$ Mpc$^3$ is essential to overcome cosmic variance. Since the current data have not reached the full depth expected for the HSC-SSP, the color cut in i-NB816 or z-NB921 induces a bias towards star-forming galaxies with large equivalent widths, primarily seen in the stellar mass functions for the H$��$ emitters at z ~ 0.25--0.40. Even so, the emission-line galaxies clearly cover a wide range of luminosity, stellar mass, and environment, thus demonstrating the usefulness of the NB data from the HSC-SSP to investigate star-forming galaxies at z, 28 pages, 22 figures, 5 tables, accepted for publication in PASJ (Subaru HSC-SSP special issue), The catalogs will be available at https://hsc-release.mtk.nao.ac.jp/
Published: 2017
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19. An optically-selected cluster catalog at redshift 0.1

Author: Oguri, Masamune, Lin, Yen-Ting, Lin, Sheng-Chieh, Nishizawa, Atsushi J., More, Anupreeta, More, Surhud, Hsieh, Bau-Ching, Medezinski, Elinor, Miyatake, Hironao, Jian, Hung-Yu, Lin, Lihwai, Takada, Masahiro, Okabe, Nobuhiro, Speagle, Joshua S., Coupon, Jean, Leauthaud, Alexie, Lupton, Robert H., Miyazaki, Satoshi, Price, Paul A., Tanaka, Masayuki, Chiu, I-Non, Komiyama, Yutaka, Okura, Yuki, Tanaka, Manobu M., and Usuda, Tomonori
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences
Abstract: We present an optically-selected cluster catalog from the Hyper Suprime-Cam (HSC) Subaru Strategic Program. The HSC images are sufficiently deep to detect cluster member galaxies down to $M_*\sim 10^{10.2}M_\odot$ even at $z\sim 1$, allowing a reliable cluster detection at such high redshifts. We apply the CAMIRA algorithm to the HSC Wide S16A dataset covering $\sim 232$ deg$^2$ to construct a catalog of 1921 clusters at redshift $0.115$ that roughly corresponds to $M_{\rm 200m}\gtrsim 10^{14}h^{-1}M_\odot$. We confirm good cluster photometric redshift performance, with the bias and scatter in $��z/(1+z)$ being better than 0.005 and 0.01 over most of the redshift range, respectively. We compare our cluster catalog with large X-ray cluster catalogs from XXL and XMM-LSS surveys and find good correlation between richness and X-ray properties. We also study the miscentering effect from the distribution of offsets between optical and X-ray cluster centers. We confirm the high ($>0.9$) completeness and purity for high mass clusters by analyzing mock galaxy catalogs., 18 pages, 18 figures, accepted for publication in PASJ; cluster catalogs are available at http://www.slac.stanford.edu/~oguri/cluster/
Published: 2017
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20. GOLDRUSH. III. A Systematic Search of Protoclusters at $z\sim4$ Based on the $>100\,\mathrm{deg^2}$ Area

Author: Toshikawa, Jun, Uchiyama, Hisakazu, Kashikawa, Nobunari, Ouchi, Masami, Overzier, Roderik, Ono, Yoshiaki, Harikane, Yuichi, Ishikawa, Shogo, Kodama, Tadayuki, Matsuda, Yuichi, Lin, Yen-Ting, Onoue, Masafusa, Tanaka, Masayuk, Nagao, Tohru, Akiyama, Masayuki, Komiyama, Yutaka, Goto, Tomotsugu, and Lee, Chien-Hsiu
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences
Abstract: We conduct a systematic search for galaxy protoclusters at $z\sim3.8$ based on the latest internal data release (S16A) of the Hyper SuprimeCam Subaru strategic program (HSC-SSP). In the Wide layer of the HSC-SSP, we investigate the large-scale projected sky distribution of $g$-dropout galaxies over an area of $121\,\mathrm{deg^2}$, and identify 216 large-scale overdense regions ($>4��$ overdensity significance) that are good protocluster candidates. Of these, 37 are located within $8\,\mathrm{arcmin}$ ($3.4\,\mathrm{physicalMpc}$) from other protocluster candidates of higher overdensity, and are expected to merge into a single massive structure by $z=0$. Therefore, we find 179 unique protocluster candidates in our survey. A cosmological simulation that includes projection effects predicts that more than 76\% of these candidates will evolve into galaxy clusters with halo masses of at least $10^{14}\,M_{\odot}$ by $z=0$. The unprecedented size of our protocluster candidate catalog allowed us to perform, for the first time, an angular clustering analysis of the systematic sample of protocluster candidates. We find a correlation length of $35.0\,h^{-1}\,\mathrm{Mpc}$. The relation between correlation length and number density of $z\sim3.8$ protocluster candidates is consistent with the prediction of the $��$CDM model, and the correlation length is similar to that of rich clusters in the local universe. This result suggests that our protocluster candidates are tracing similar spatial structures as those expected of the progenitors of rich clusters and enhances the confidence that our method to identify protoclusters at high redshifts is robust. In the coming years, our protocluster search will be extended to the entire HSC-SSP Wide sky coverage of $\sim1400\,\mathrm{deg^2}$ to probe cluster formation over a wide redshift range of $z\sim2\mathrm{-}6$., 11 pages, 8 figures, accepted for publication in PASJ special issue
Published: 2017
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21. First results on the cluster galaxy population from the Subaru Hyper Suprime-Cam survey. II. Faint end color-magnitude diagrams and radial profiles of red and blue galaxies at $0.1

Author: Nishizawa, Atsushi J., Oguri, Masamue, Oogi, Taira, More, Surhud, Nishimichi, Takahiro, Nagashima, Masahiro, Lin, Yen-Ting, Mandelbaum, Rachel, Takada, Masahiro, Bahcall, Neta, Coupon, Jean, Huang, Song, Jian, Hung-Yu, Komiyama, Yutaka, Leauthaud, Alexie, Lin, Lihwai, Miyatake, Hironao, Miyazaki, Satoshi, and Tanaka, Masayuki
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present a statistical study of the redshift evolution of the cluster galaxy population over a wide redshift range from 0.1 to 1.1, using $\sim 1900$ optically-selected CAMIRA clusters from $\sim 232$~deg$^2$ of the Hyper Suprime-Cam (HSC) Wide S16A data. Our stacking technique with a statistical background subtraction reveals color-magnitude diagrams of red-sequence and blue cluster galaxies down to faint magnitudes of $m_z\sim 24$. We find that the linear relation of red-sequence galaxies in the color-magnitude diagram extends down to the faintest magnitudes we explore with a small intrinsic scatter $��_{\rm int}(g-r), 18pages, 10 figures, accepted as PASJ special issue
Published: 2017
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22. The SDSS-IV extended baryon oscillation spectroscopic survey: Overview and early data

Author: Dawson, Kyle S, Kneib, Jean-Paul, Percival, Will J, Alam, Shadab, Albareti, Franco D, Anderson, Scott F, Armengaud, Eric, Aubourg, Éric, Bailey, Stephen, Bautista, Julian E, Berlind, Andreas A, Bershady, Matthew A, Beutler, Florian, Bizyaev, Dmitry, Blanton, Michael R, Blomqvist, Michael, Bolton, Adam S, Bovy, Jo, Brandt, WN, Brinkmann, Jon, Brownstein, Joel R, Burtin, Etienne, Busca, NG, Cai, Zheng, Chuang, Chia-Hsun, Clerc, Nicolas, Comparat, Johan, Cope, Frances, Croft, Rupert AC, Cruz-Gonzalez, Irene, da Costa, Luiz N, Cousinou, Marie-Claude, Darling, Jeremy, de la Macorra, Axel, de la Torre, Sylvain, Delubac, Timothée, du Mas des Bourboux, Hélion, Dwelly, Tom, Ealet, Anne, Eisenstein, Daniel J, Eracleous, Michael, Escoffier, S, Fan, Xiaohui, Finoguenov, Alexis, Font-Ribera, Andreu, Frinchaboy, Peter, Gaulme, Patrick, Georgakakis, Antonis, Green, Paul, Guo, Hong, Guy, Julien, Ho, Shirley, Holder, Diana, Huehnerhoff, Joe, Hutchinson, Timothy, Jing, Yipeng, Jullo, Eric, Kamble, Vikrant, Kinemuchi, Karen, Kirkby, David, Kitaura, Francisco-Shu, Klaene, Mark A, Laher, Russ R, Lang, Dustin, Laurent, Pierre, Le Goff, Jean-Marc, Li, Cheng, Liang, Yu, Lima, Marcos, Lin, Qiufan, Lin, Weipeng, Lin, Yen-Ting, Long, Daniel C, Lundgren, Britt, MacDonald, Nicholas, Maia, Marcio Antonio Geimba, Malanushenko, Elena, Malanushenko, Viktor, Mariappan, Vivek, McBride, Cameron K, McGreer, Ian D, Ménard, Brice, Merloni, Andrea, Meza, Andres, Montero-Dorta, Antonio D, Muna, Demitri, Myers, Adam D, Nandra, Kirpal, Naugle, Tracy, Newman, Jeffrey A, Noterdaeme, Pasquier, Nugent, Peter, Ogando, Ricardo, Olmstead, Matthew D, Oravetz, Audrey, Oravetz, Daniel J, Padmanabhan, Nikhil, Palanque-Delabrouille, Nathalie, Pan, Kaike, and Parejko, John K
Subjects: surveys, astro-ph.CO, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Astrophysics::Galaxy Astrophysics, observations [cosmology], Astronomical and Space Sciences
Abstract: In a six-year program started in 2014 July, the Extended Baryon Oscillation Spectroscopic Survey (eBOSS) will conduct novel cosmological observations using the BOSS spectrograph at Apache Point Observatory. These observations will be conducted simultaneously with the Time Domain Spectroscopic Survey (TDSS) designed for variability studies and the Spectroscopic Identification of eROSITA Sources (SPIDERS) program designed for studies of X-ray sources. In particular, eBOSS will measure with percent-level precision the distance-redshift relation with baryon acoustic oscillations (BAO) in the clustering of matter. eBOSS will use four different tracers of the underlying matter density field to vastly expand the volume covered by BOSS and map the large-scale-structures over the relatively unconstrained redshift range 0.6 < z < 2.2. Using more than 250,000 new, spectroscopically confirmed luminous red galaxies at a median redshift z = 0.72, we project that eBOSS will yield measurements of the angular diameter distance dA(z) to an accuracy of 1.2% and measurements of H(z) to 2.1% when combined with the z > 0.6 sample of BOSS galaxies. With ∼195,000 new emission line galaxy redshifts, we expect BAO measurements of dA(z) to an accuracy of 3.1% and H(z) to 4.7% at an effective redshift of z = 0.87. A sample of more than 500,000 spectroscopically confirmed quasars will provide the first BAO distance measurements over the redshift range 0.9 < z < 2.2, with expected precision of 2.8% and 4.2% on dA(z) and H(z), respectively. Finally, with 60,000 new quasars and re-observation of 60,000 BOSS quasars, we will obtain new Lyα forest measurements at redshifts z > 2.1; these new data will enhance the precision of dA(z) and H(z) at z > 2.1 by a factor of 1.44 relative to BOSS. Furthermore, eBOSS will provide improved tests of General Relativity on cosmological scales through redshift-space distortion measurements, improved tests for non-Gaussianity in the primordial density field, and new constraints on the summed mass of all neutrino species. Here, we provide an overview of the cosmological goals, spectroscopic target sample, demonstration of spectral quality from early data, and projected cosmological constraints from eBOSS.
Published: 2016

23. Clinical Results After Prostatic Artery Embolization Using the PErFecTED Technique: A Single-Center Study

Author: Helena Pereira, Olivier Pellerin, Marc Sapoval, Lin Yen-Ting, Nicolas Thiounn, Gregory Amouyal, Gilles Chatellier, Costantino Del Giudice, and Carole Déan
Subjects: Retrograde ejaculation, Male, medicine.medical_specialty, medicine.medical_treatment, 030232 urology & nephrology, Prostatic Hyperplasia, Single Center, 030218 nuclear medicine & medical imaging, 03 medical and health sciences, 0302 clinical medicine, Lower Urinary Tract Symptoms, Lower urinary tract symptoms, Prostate, medicine, Humans, Radiology, Nuclear Medicine and imaging, Embolization, Aged, Retrospective Studies, Aged, 80 and over, business.industry, Retrospective cohort study, Arteries, Middle Aged, medicine.disease, Embolization, Therapeutic, Prostatic artery embolization, Surgery, medicine.anatomical_structure, Treatment Outcome, Prostate surgery, Radiology, Cardiology and Cardiovascular Medicine, business
Abstract: Prostatic artery embolization (PAE) has been performed for a few years, but there is no report on PAE using the PErFecTED technique outside from the team that initiated this approach. This single-center retrospective open label study reports our experience and clinical results on patients suffering from symptomatic BPH, who underwent PAE aiming at using the PErFecTED technique. We treated 32 consecutive patients, mean age 65 (52–84 years old) between December 2013 and January 2015. Patients were referred for PAE after failure of medical treatment and refusal or contra-indication to surgery. They were treated using the PErFecTED technique, when feasible, with 300–500 µm calibrated microspheres (two-night hospital stay or outpatient procedure). Follow-up was performed at 3, 6, and 12 months. We had a 100 % immediate technical success of embolization (68 % of feasibility of the PErFecTED technique) with no immediate complications. After a mean follow-up of 7.7 months, we observed a 78 % rate of clinical success. Mean IPSS decreased from 15.3 to 4.2 (p = .03), mean QoL from 5.4 to 2 (p = .03), mean Qmax increased from 9.2 to 19.2 (p = .25), mean prostatic volume decreased from 91 to 62 (p = .009) mL. There was no retrograde ejaculation and no major complication. PAE using the PErFecTED technique is a safe and efficient technique to treat bothersome LUTS related to BPH. It is of interest to note that the PErFecTED technique cannot be performed in some cases for anatomical reasons.
Published: 2015

24. The $z < 1.2$ optical luminosity function from a sample of $\sim410 \, 000$ galaxies in bootes

Author: Beare, Richard A., Brown, Michael J. I., Pimbblet, Kevin A., Bian, Fuyan, and Lin, Yen-Ting
Subjects: Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Using a sample of ~410 000 galaxies to depth I_AB = 24 over 8.26 deg^2 in the Bootes field (~10 times larger than z~1 luminosity function studies in the prior literature), we have accurately measured the evolving B-band luminosity function of red galaxies at z, 21 pages, 21 figures
Published: 2015
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25. The Massive and Distant Clusters of WISE Survey: MOO J1142+1527, A 10$^{15}$ M$_\odot$ Galaxy Cluster at z=1.19

Author: Gonzalez, Anthony H., Decker, Bandon, Brodwin, Mark, Eisenhardt, Peter R. M., Marrone, Daniel P., Stanford, S. A., Stern, Daniel, Wylezalek, Dominika, Aldering, Greg, Abdulla, Zubair, Boone, Kyle, Carlstrom, John, Fagrelius, Parker, Gettings, Daniel P., Greer, Christopher H., Hayden, Brian, Leitch, Erik M., Lin, Yen-Ting, Mantz, Adam B., Muchovej, Stephen, Perlmutter, Saul, and Zeimann, Gregory R.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present confirmation of the cluster MOO J1142+1527, a massive galaxy cluster discovered as part of the Massive and Distant Clusters of WISE Survey. The cluster is confirmed to lie at $z=1.19$, and using the Combined Array for Research in Millimeter-wave Astronomy we robustly detect the Sunyaev-Zel'dovich (SZ) decrement at 13.2$\sigma$. The SZ data imply a mass of $\mathrm{M}_{200m}=(1.1\pm0.2)\times10^{15}$ $\mathrm{M}_\odot$, making MOO J1142+1527 the most massive galaxy cluster known at $z>1.15$ and the second most massive cluster known at $z>1$. For a standard $\Lambda$CDM cosmology it is further expected to be one of the $\sim 5$ most massive clusters expected to exist at $z\ge1.19$ over the entire sky. Our ongoing Spitzer program targeting $\sim1750$ additional candidate clusters will identify comparably rich galaxy clusters over the full extragalactic sky., Comment: Submitted to ApJ Letters, 6 pages, 4 figures
Published: 2015
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26. Star Formation at $4 < z < 6$ From the Spitzer Large Area Survey with Hyper-Suprime-Cam (SPLASH)

Author: Steinhardt, Charles L., Speagle, Josh S., Capak, Peter, Silverman, John D., Carollo, Marcella, Dunlop, James, Hashimoto, Yasuhiro, Hsieh, Bau-Ching, Ilbert, Olivier, Fevre, Olivier Le, Floc'h, Emeric Le, Lee, Nicholas, Lin, Liwhai, Lin, Yen-Ting, Masters, Daniel, McCracken, Henry J., Nagao, Tohru, Petric, Andreea, Salvato, Mara, Sanders, Dave, Scoville, Nick, Sheth, Kartik, Strauss, Michael A., and Taniguchi, Yoshiaki
Subjects: Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Using the first 50% of data collected for the Spitzer Large Area Survey with Hyper-Suprime-Cam (SPLASH) observations on the 1.8 deg$^2$ Cosmological Evolution Survey (COSMOS) we estimate the masses and star formation rates of 3398 $M_*>10^{10}M_\odot $ star-forming galaxies at $4 < z < 6$ with a substantial population up to $M_* \gtrsim 10^{11.5} M_\odot$. We find that the strong correlation between stellar mass and star formation rate seen at lower redshift (the "main sequence" of star-forming galaxies) extends to $z\sim6$. The observed relation and scatter is consistent with a continued increase in star formation rate at fixed mass in line with extrapolations from lower-redshift observations. It is difficult to explain this continued correlation, especially for the most massive systems, unless the most massive galaxies are forming stars near their Eddington-limited rate from their first collapse. Furthermore, we find no evidence for moderate quenching at higher masses, indicating quenching either has not occurred prior to $z \sim 6$ or else occurs rapidly, so that few galaxies are visible in transition between star-forming and quenched., ApJL, accepted
Published: 2014
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27. A Quasi-Experiment on Computer Multimedia Integration into AIDS Education

Author: Tsai Chia-Wen, Shen Pei-Di, and Lin Yen-Ting
Abstract: Keywords: Health Issues, High Schools, HIV/AIDS Education, India, Integrating Computers and Multimedia
Published: 2013
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28. On the Populations of Radio Galaxies with Extended Morphology at z<0.3

Author: Lin, Yen-Ting, Shen, Yue, Strauss, Michael, Richards, Gordon, and Lunnan, Ragnhild
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Extended extragalactic radio sources have traditionally been classified into FR I and II types, based on the ratio r of the separation S between the brightest regions on either sides of the host galaxy and the total size T of the radio source. Here we examine the distribution of various physical properties as a function of r of 1040 luminous radio galaxies (RGs) at z0.8 AND OIII5007 line luminosity >10^6 Lsun are markedly different on average from the rest of the RGs, in the sense that they are hosted in lower mass galaxies, live in relatively sparse environments, and have higher accretion rates onto the central SMBH. Thus these objects and the rest of RGs form a well-defined dichotomy. Motivated by the stark differences in the nuclear emission line properties of the RG subsamples, we suggest that the accretion rate onto the SMBH may play the primary role in creating the different morphologies. At relatively high accretion rates, the accretion system may produce powerful jets that create the "classical double" morphology (roughly corresponding to the LD sources with r>0.8 and emission lines); at lower accretion rates the jets from a radiatively inefficient accretion flow generate radio lobes without apparent "hot spots" at the edge (corresponding to the majority of LD sources). At slightly lower accretion rates AND in galaxies with dense galactic structure, sources with prominent jets result. It is possible that while the high accretion rate systems could affect sub-Mpc scale environments, the jets from lower accretion rate systems may efficiently suppress activity within the host galaxies., ApJ, accepted. 20 pages, 16 figures, 4 tables. Image quality of Figures 1 & 2 degraded due to size limits. Table 4 is available and kept up-to-date at http://member.ipmu.jp/yen-ting.lin/RG/index.html. Higher resolution version available at http://member.ipmu.jp/yen-ting.lin/Data/ytlin.pdf
Published: 2010
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29. WMAP constraints on the Intra-Cluster Medium

Author: Afshordi, Niayesh, Lin, Yen-Ting, and Sanderson, Alastair J. R.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract: We devise a Monte-Carlo based, optimized filter match method to extract the thermal Sunyaev-Zel'dovich (SZ) signature of a catalog of 116 low-redshift X-ray clusters from the first year data release of the Wilkinson Microwave Anisotropy Probe (WMAP). We detect an over-all amplitude for the SZ signal at the ~ 8-sigma level, yielding a combined constraint of f_{gas}h = 0.08 +/- 0.01 (ran) +/- 0.01 (sys) on the gas mass fraction of the Intra-Cluster Medium. We also compile X-ray estimated gas fractions from the literature for our sample, and find that they are consistent with the SZ estimates at the 2-sigma level, while both show an increasing trend with X-ray temperature. Nevertheless, our SZ estimated gas fraction is 30-40% smaller than the concordance LCDM cosmic average. We also express our observations in terms of the SZ flux-temperature relation, and compare it with other observations, as well as numerical studies. Based on its spectral and spatial signature, we can also extract the microwave point source signal of the clusters at the 3-sigma level, which puts the average microwave luminosity (at ~ 41 GHz) of bright cluster members (M_K < -21) at (2.4 +/- 0.8) x 10^{27} h^{-2} erg/s/Hz. Furthermore, we can constrain the average dark matter halo concentration parameter to c_{vir}=3.4+0.6-0.9, for clusters with T_x > 5 kev. Our work serves as an example for how correlation of SZ surveys with cluster surveys in other frequencies can significantly increase our physical understanding of the intra-cluster medium., 34 pages, 6 ps figures, Extended discussion of theoretical uncertainties, radio sources, and future prospects, Accepted for Publication in ApJ
Published: 2004
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30. THE EIGHTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY: FIRST DATA FROM SDSS-III

Author: collaboration, SDSS-III, Aihara, Hiroaki, Prieto, Carlos Allende, An, Deokkeun, Anderson, Scott F., Aubourg, Éric, Balbinot, Eduardo, Beers, Timothy C., Berlind, Andreas A., Bickerton, Steven J., Bizyaev, Dmitry, Blanton, Michael R., Bochanski, John J., Bolton, Adam S., Bovy, Jo, Brandt, W. N., Brinkmann, J., Brown, Peter J., Brownstein, Joel R., Busca, Nicolas G., Campbell, Heather, Carr, Michael A., Chen, Yanmei, Chiappini, Cristina, Comparat, Johan, Connolly, Natalia, Cortes, Marina, Croft, Rupert A. C., Cuesta, Antonio J., da Costa, Luiz N., Davenport, James R. A., Dawson, Kyle, Dhital, Saurav, Ealet, Anne, Ebelke, Garrett L., Edmondson, Edward M., Eisenstein, Daniel J., Escoffier, Stephanie, Esposito, Massimiliano, Evans, Michael L., Fan, Xiaohui, Castellá, Bruno Femení a, Font-Ribera, Andreu, Frinchaboy, Peter M., Ge, Jian, Gillespie, Bruce A., Gilmore, G., Hernández, Jonay I. González, Gott, J. Richard, Gould, Andrew, Grebel, Eva K., Gunn, James E., Hamilton, Jean-Christophe, Harding, Paul, Harris, David W., Hawley, Suzanne L., Hearty, Frederick R., Ho, Shirley, Hogg, David W., Holtzman, Jon A., Honscheid, Klaus, Inada, Naohisa, Ivans, Inese I., Jiang, Linhua, Johnson, Jennifer A., Jordan, Cathy, Jordan, Wendell P., Kazin, Eyal A., Kirkby, David, Klaene, Mark A., Knapp, G. R., Kneib, Jean-Paul, Kochanek, C. S., Koesterke, Lars, Kollmeier, Juna A., Kron, Richard G., Lampeitl, Hubert, Lang, Dustin, Goff, Jean-Marc Le, Lee, Young Sun, Lin, Yen-Ting, Long, Daniel C., Loomis, Craig P., Lucatello, Sara, Lundgren, Britt, Lupton, Robert H., Ma, Zhibo, MacDonald, Nicholas, Mahadevan, Suvrath, Maia, Marcio A. G., Makler, Martin, Malanushenko, Elena, Malanushenko, Viktor, Mandelbaum, Rachel, Maraston, Claudia, Margala, Daniel, Masters, Karen L., McBride, Cameron K., McGehee, Peregrine M., McGreer, Ian D., Ménard, Brice, Miralda-Escudé, Jordi, Morrison, Heather L., Mullally, F., Muna, Demitri, Munn, Jeffrey A., Murayama, Hitoshi, Myers, Adam D., Naugle, Tracy, Neto, Angelo Fausti, Nguyen, Duy Cuong, Nichol, Robert C., O'Connell, Robert W., Ogando, Ricardo L. C., Olmstead, Matthew D., Oravetz, Daniel J., Padmanabhan, Nikhil, Palanque-Delabrouille, Nathalie, Pan, Kaike, Pandey, Parul, Pâris, Isabelle, Percival, Will J., Petitjean, Patrick, Pfaffenberger, Robert, Pforr, Janine, Phleps, Stefanie, Pichon, Christophe, Pieri, Matthew M., Prada, Francisco, Price-Whelan, Adrian M., Raddick, M. Jordan, Ramos, Beatriz H. F., Reylé, Céline, Rich, James, Richards, Gordon T., Rix, Hans-Walter, Robin, Annie C., Rocha-Pinto, Helio J., Rockosi, Constance M., Roe, Natalie A., Rollinde, Emmanuel, Ross, Ashley J., Ross, Nicholas P., Rossetto, Bruno M., Sánchez, Ariel G., Sayres, Conor, Schlegel, David J., Schlesinger, Katharine J., Schmidt, Sarah J., Schneider, Donald P., Sheldon, Erin, Shu, Yiping, Simmerer, Jennifer, Simmons, Audrey E., Sivarani, Thirupathi, Snedden, Stephanie A., Sobeck, Jennifer S., Steinmetz, Matthias, Strauss, Michael A., Szalay, Alexander S., Tanaka, Masayuki, Thakar, Aniruddha R., Thomas, Daniel, Tinker, Jeremy L., Tofflemire, Benjamin M., Tojeiro, Rita, Tremonti, Christy A., Vandenberg, Jan, Magaña, M. Vargas, Verde, Licia, Vogt, Nicole P., Wake, David A., Wang, Ji, Weaver, Benjamin A., Weinberg, David H., White, Martin, White, Simon D. M., Yanny, Brian, Yasuda, Naoki, Yeche, Christophe, Zehavi, Idit, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), SDSS-III, Universitat de Barcelona, Instituto de Astrofisica de Canarias (IAC), EWHA Womans University (EWHA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], Department of Physics and Astronomy [East Lansing], Michigan State University [East Lansing], Michigan State University System-Michigan State University System, Apache point observatory, Department of Astronomy and Astrophysics [PennState], Pennsylvania State University (Penn State), Penn State System-Penn State System, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), and Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Gravitation, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], media_common.quotation_subject, Metallicity, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astronomical spectroscopy, surveys, Observacions astronòmiques, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, Cosmologia, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Quasar, Celestial sphere, Espectroscòpia, Spectrum analysis, Galaxy, Cosmology, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], atlases, Radial velocity, Stars, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], 13. Climate action, Space and Planetary Science, Sky, 95.80.+p Astronomical catalogs, atlases, sky surveys, databases, retrieval systems, archives, etc. 98.62.Ra Intergalactic matter, quasar absorption and emission-line systems, Lyman forest 95.85.Kr Visible (390-750 nm) 98.54.Aj Quasa, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Instrumentation and Methods for Astrophysics, catalogs, Astronomical observations
Abstract: The Sloan Digital Sky Survey (SDSS) started a new phase in August 2008, with new instrumentation and new surveys focused on Galactic structure and chemical evolution, measurements of the baryon oscillation feature in the clustering of galaxies and the quasar Ly alpha forest, and a radial velocity search for planets around ~8000 stars. This paper describes the first data release of SDSS-III (and the eighth counting from the beginning of the SDSS). The release includes five-band imaging of roughly 5200 deg^2 in the Southern Galactic Cap, bringing the total footprint of the SDSS imaging to 14,555 deg^2, or over a third of the Celestial Sphere. All the imaging data have been reprocessed with an improved sky-subtraction algorithm and a final, self-consistent photometric recalibration and flat-field determination. This release also includes all data from the second phase of the Sloan Extension for Galactic Understanding and Evolution (SEGUE-2), consisting of spectroscopy of approximately 118,000 stars at both high and low Galactic latitudes. All the more than half a million stellar spectra obtained with the SDSS spectrograph have been reprocessed through an improved stellar parameters pipeline, which has better determination of metallicity for high metallicity stars., Astrophysical Journal Supplements, in press (minor updates from submitted version)
Published: 2011
Full Text: View/download PDF

31. The Detailed Science Case for the Maunakea Spectroscopic Explorer: the Composition and Dynamics of the Faint Universe

Author: Mcconnachie, Alan, Babusiaux, Carine, Balogh, Michael, Driver, Simon, Côté, Pat, Courtois, Helene, Davies, Luke, Ferrarese, Laura, Gallagher, Sarah, Ibata, Rodrigo, Martin, Nicolas, Robotham, Aaron, Venn, Kim, Villaver, Eva, Bovy, Jo, Boselli, Alessandro, Colless, Matthew, Comparat, Johan, Denny, Kelly, Duc, Pierre-Alain, Ellison, Sara, Grijs, Richard, Fernandez-Lorenzo, Mirian, Freeman, Ken, Guhathakurta, Raja, Hall, Patrick, Hopkins, Andrew, Hudson, Mike, Johnson, Andrew, Kaiser, Nick, Koda, Jun, Konstantopoulos, Iraklis, Koshy, George, Lee, Khee-Gan, Nusser, Adi, Pancoast, Anna, Peng, Eric, Peroux, Celine, Petitjean, Patrick, Pichon, Christophe, Poggianti, Bianca, Schmid, Carlo, Shastri, Prajval, Shen, Yue, Willot, Chris, Croom, Scott, Lallement, Rosine, Schimd, Carlo, Smith, Dan, Walker, Matthew, Willis, Jon, Colless, Alessandro Bosselli Matthew, Goswami, Aruna, Jarvis, Matt, Jullo, Eric, Kneib, Jean-Paul, Konstantopoloulous, Iraklis, Newman, Jeff, Richard, Johan, Sutaria, Firoza, Taylor, Edwar, Waerbeke, Ludovic, Battaglia, Giuseppina, Hall, Pat, Haywood, Misha, Sakari, Charli, Seibert, Arnaud, Thirupathi, Sivarani, Wang, Yuting, Wang, Yiping, Babas, Ferdinand, Bauman, Steve, Caffau, Elisabetta, Laychak, Mary Beth, Crampton, David, Devost, Daniel, Flagey, Nicolas, Han, Zhanwen, Higgs, Clare, Hill, Vanessa, Ho, Kevin, Isani, Sidik, Mignot, Shan, Murowinski, Rick, Pandey, Gajendra, Salmon, Derrick, Siebert, Arnaud, Simons, Doug, Starkenburg, Else, Szeto, Kei, Tully, Brent, Vermeulen, Tom, Withington, Kanoa, Arimoto, Nobuo, Asplund, Martin, Aussel, Herve, Bannister, Michele, Bhatt, Harish, Bhargavi, Ss, Blakeslee, John, Bland-Hawthorn, Joss, Bullock, James, Burgarella, Denis, Chang, Tzu-Ching, Cole, Andrew, Cooke, Jeff, Cooper, Andrew, Di Matteo, Paola, Favole, Ginevra, Flores, Hector, Gaensler, Bryan, Garnavich, Peter, Karoline Gilbert, Gonzalez-Delgado, Rosa, Guhathakurta, Puragra, Hasinger, Guenther, Herwig, Falk, Hwang, Narae, Jablonka, Pascale, Jarvis, Matthew, Kamath, Umanath, Kewley, Lisa, Le Borgne, Damien, Lewis, Geraint, Lupton, Robert, Martell, Sarah, Mateo, Mario, Mena, Olga, Nataf, David, Newman, Jeffrey, Pérez, Enrique, Prada, Francisco, Puech, Mathieu, Recio-Blanco, Alejandra, Robin, Annie, Saunders, Will, Smith, Daniel, Stalin, C. S., Tao, Charling, Thanjuvur, Karun, Tresse, Laurence, Waerbeke, Ludo, Wang, Jian-Min, Yong, David, Zhao, Gongbo, Boisse, Patrick, Bolton, James, Bonifacio, Piercarlo, Bouchy, Francois, Cowie, Len, Cunha, Katia, Deleuil, Magali, Mooij, Ernst, Dufour, Patrick, Foucaud, Sebastien, Glazebrook, Karl, Hutchings, John, Kobayashi, Chiaki, Kudritzki, Rolf-Peter, Li, Yang-Shyang, Lin, Lihwai, Lin, Yen-Ting, Makler, Martin, Narita, Norio, Park, Changbom, Ransom, Ryan, Ravindranath, Swara, Eswar Reddy, Bacham, Sawicki, Marcin, Simard, Luc, Srianand, Raghunathan, Storchi-Bergmann, Thaisa, Umetsu, Keiichi, Wang, Ting-Gui, Woo, Jong-Hak, Wu, Xue-Bing, Institut de Physique Nucléaire de Lyon (IPNL), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), NRC Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autónoma de Madrid (UAM), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Cornell Lab of Ornithology, Cornell University [New York], Recherches Epistémologiques et Historiques sur les Sciences Exactes et les Institutions Scientifiques (REHSEIS (UMR_7596)), Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), University of Edinburgh, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), CSIRO Digital Productivity Flagship, Public Health Agency of Canada, Laboratoire d'Astrophysique de Toulouse-Tarbes, École normale supérieure - Lyon (ENS Lyon)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées, Department of Electrical and Computer Engineering [Minneapolis] (ECE), University of Minnesota [Twin Cities] (UMN), University of Minnesota System-University of Minnesota System, Herzberg Institute of Astrophysics, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Department of electronic engineering, Chang Gung University, Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), Anglo-Australian Observatory (AAO), AUTRES, Instituto de Fisica Corpuscular (IFIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universitat de València (UV), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Cosmological Impact of the First Stars (CIFIST), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Département de médecine oncologique, CRLCC Paul Strauss, Centre for Astrophysics and Supercomputing [Swinburne] (CAS), Swinburne University of Technology [Melbourne], Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Department of Chemical and Biomolecular Engineering, School of Physics, Korea Institute for Advanced Study (KIAS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Études des Structures, des Processus d’Adaptation et des Changements de l’Espace (ESPACE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Avignon Université (AU)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Universidad Autonoma de Madrid (UAM), Cornell University, Recherches Epistémologiques et Historiques sur les Sciences Exactes et les Institutions Scientifiques (REHSEIS), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), University of Minnesota [Twin Cities], Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Universitat de València (UV), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), PSL Research University (PSL)-PSL Research University (PSL), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Cornell Laboratory of Ornithology, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), and Cornell Lab of Ornithology [New York]
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Astrophysics of Galaxies, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics
Abstract: MSE is an 11.25m aperture observatory with a 1.5 square degree field of view that will be fully dedicated to multi-object spectroscopy. More than 3200 fibres will feed spectrographs operating at low (R ~ 2000 - 3500) and moderate (R ~ 6000) spectral resolution, and approximately 1000 fibers will feed spectrographs operating at high (R ~ 40000) resolution. MSE is designed to enable transformational science in areas as diverse as tomographic mapping of the interstellar and intergalactic media; the in-situ chemical tagging of thick disk and halo stars; connecting galaxies to their large scale structure; measuring the mass functions of cold dark matter sub-halos in galaxy and cluster-scale hosts; reverberation mapping of supermassive black holes in quasars; next generation cosmological surveys using redshift space distortions and peculiar velocities. MSE is an essential follow-up facility to current and next generations of multi-wavelength imaging surveys, including LSST, Gaia, Euclid, WFIRST, PLATO, and the SKA, and is designed to complement and go beyond the science goals of other planned and current spectroscopic capabilities like VISTA/4MOST, WHT/WEAVE, AAT/HERMES and Subaru/PFS. It is an ideal feeder facility for E-ELT, TMT and GMT, and provides the missing link between wide field imaging and small field precision astronomy. MSE is optimized for high throughput, high signal-to-noise observations of the faintest sources in the Universe with high quality calibration and stability being ensured through the dedicated operational mode of the observatory. (abridged), Comment: 210 pages, 91 figures. Exposure draft. Appendices to the Detailed Science Case can be found at http://mse.cfht.hawaii.edu/docs/

32. SpIES: The Spitzer-IRAC Equatorial Survey

Author: Richards, Gordon, Lacy, Mark, Strauss, Michael, Spergel, David, Anderson, Scott, Bauer, Franz, Bochanski, John, Brandt, Niel, Cushing, Michael, Fan, Xiaohui, Gallagher, Sarah, Glikman, Eilat, Haggard, Daryl, Hewett, Paul, Hodge, Jaqueline, Hopkins, Philip, Hughes, Jack, Jiang, Linhua, Knapp, Gillian, Kneib, Jean-Paul, Lin, Yen-Ting, Lupton, Robert, Makler, Martin, Mcgehee, Peregrine, Mcmahon, Richard, Menanteau, Felipe, Myers, Adam, Nichol, Robert, Ross, Nic, Ryan, Erin, Schneider, Donald, Szalay, Alex, Meg Urry, Viero, Marco, Warren, Stephen, and Zakamska, Nadia

33. SPLASH: Spitzer Large Area Survey with Hyper-Suprime-Cam

Author: Capak, Peter, Aussel, Herve, Bundy, Kevin, Bethermin, Matthieu, Carollo, Marcella, Ram-Chary, Ranga, Civano, Francesca, Coupon, Jean, Diener, Catrina, Donley, Jennifer, Dunlop, Jim, Elvis, Martin, Faisst, Andreas, Foucaud, Sebastien, Green, Jenny, Gunn, Jim, Hashimoto, Yasuhiro, Hassinger, Gunther, Hsieh, Bau-Ching, Huang, Lijin, Ilbert, Olivier, Lefloc H, Emeric, Lefevre, Olivier, Lilly, Simon, Lin, Lihwai, Lin, Yen-Ting, Miyazaki, Satoshi, Mobasher, Bahram, Moriya, Takashi, Nagao, Tohru, Ono, Yoshiaki, Ouchi, Massami, Petric, Andrea, Pych, Wojtek, Quimby, Robert, Saito, Tomoki, Salvato, Mara, Sanders, Dave, Scarlata, Claudia, Eva Schinnerer, Scoville, Nick, Sheth, Kartik, Shimasaku, Kazuhiro, Silverman, John, Smolcic, Vernesa, Steinhardt, Charles, Strauss, Michael, Surace, Jason, Tanaka, Masaomi, Tanaka, Massayuki, Taniguchi, Yoshi, Teplitz, Harry, Toshida, Naoki, Wang, Wei-Hao, and Urata, Yuji

34. The Thirteenth Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the SDSS-IV Survey MApping Nearby Galaxies at Apache Point Observatory

Author: Sdss, Collaboration, Albareti, Franco D., Allende Prieto, Carlos, Almeida, Andres, Anders, Friedrich, Anderson, Scott, Andrews, Brett H., Aragon-Salamanca, Alfonso, Argudo-Fernandez, Maria, Armengaud, Eric, Aubourg, Eric, Avila-Reese, Vladimir, Badenes, Carles, Bailey, Stephen, Barbuy, Beatriz, Barger, Kat, Barrera-Ballesteros, Jorge, Bartosz, Curtis, Basu, Sarbani, Bates, Dominic, Battaglia, Giuseppina, Baumgarten, Falk, Baur, Julien, Bautista, Julian, Beers, Timothy C., Belfiore, Francesco, Bershady, Matthew, Bertran Lis, Sara, Bird, Jonathan C., Bizyaev, Dmitry, Blanc, Guillermo A., Blanton, Michael, Blomqvist, Michael, Bolton, Adam S., Borissova, J., Bovy, Jo, Nielsen Brandt, William, Brinkmann, Jonathan, Brownstein, Joel R., Bundy, Kevin, Burtin, Etienne, Busca, Nicolas G., Orlando Camacho Chavez, Hugo, Cano Diaz, M., Cappellari, Michele, Carrera, Ricardo, Chen, Yanping, Cherinka, Brian, Edmond Cheung, Chiappini, Cristina, Chojnowski, Drew, Chuang, Chia-Hsun, Chung, Haeun, Cirolini, Rafael Fernando, Clerc, Nicolas, Cohen, Roger E., Comerford, Julia M., Comparat, Johan, Cousinou, Marie-Claude, Covey, Kevin, Crane, Jeffrey D., Croft, Rupert, Cunha, Katia, Da Costa, Luiz, Da Silva Ilha, Gabriele, Darling, Jeremy, Davidson, James W., Dawson, Kyle, Lee, Nathan, La Macorra, Axel, La Torre, Sylvain, Deconto Machado, Alice, Delubac, Timothee, Diamond-Stanic, Aleksandar M., Donor, John, Downes, Juan Jose, Drory, Niv, Du Mas Des Bourboux, Helion, Du, Cheng, Dwelly, Tom, Ebelke, Garrett, Eigenbrot, Arthur, Eisenstein, Daniel J., Elsworth, Yvonne P., Emsellem, Eric, Eracleous, Michael, Escoffier, Stephanie, Evans, Michael L., Falcon-Barroso, Jesus, Fan, Xiaohui, Favole, Ginevra, Fernandez-Alvar, Emma, Fernandez-Trincado, J. G., Feuillet, Diane, Fleming, Scott W., Font-Ribera, Andreu, Freischlad, Gordon, Frinchaboy, Peter, Fu, Hai, Gao, Yang, Garcia-Hernandez, D. A., Garcia Perez, Ana E., Garcia, Rafael A., Garcia-Dias, R., Gaulme, Patrick, Ge, Junqiang, Geisler, Douglas, Gil Marin, Hector, Gillespie, Bruce, Girardi, Leo, Goddard, Daniel, Gomez Maqueo Chew, Yilen, Gonzalez-Perez, Violeta, Grabowski, Kathleen, Green, Paul, Grier, Catherine J., Grier, Thomas, Guo, Hong, Guy, Julien, Hagen, Alex, Hall, Matt, Harding, Paul, Harley, R. E., Hasselquist, Sten, Hawley, Suzanne, Hayes, Christian R., Hearty, Fred, Hekker, Saskia, Hernandez Toledo, Hector, Ho, Shirley, Hogg, David W., Holley-Bockelmann, Kelly, Holtzman, Jon A., Holzer, Parker H., Hu, Jian, Huber, Daniel, Hutchinson, Timothy Alan, Hwang, Ho Seong, Ibarra-Medel, Hector J., Ivans, Inese I., Ivory, Keshawn, Jaehnig, Kurt, Jensen, Trey W., Johnson, Jennifer A., Jones, Amy, Jullo, Eric, Kallinger, T., Kinemuchi, Karen, Kirkby, David, Klaene, Mark, Kneib, Jean-Paul, Kollmeier, Juna A., Lacerna, Ivan, Lane, Richard R., Lang, Dustin, Laurent, Pierre, Law, David R., Le Goff, Jean-Marc, Leauthaud, Alexie, Li, Cheng, Li, Ran, Li, Chen, Li, Niu, Liang, Fu-Heng, Liang, Yu, Lima, Marcos, Lin, Lihwai, Lin, Lin, Lin, Yen-Ting, Long, Dan, Lucatello, Sara, Macdonald, Nicholas, Macleod, Chelsea L., Mackereth, J. Ted, Mahadevan, Suvrath, Antonio-Geimba Maia, Marcio, Maiolino, Roberto, Majewski, Steven R., Malanushenko, Olena, Dullius Mallmann, Nicolas, Manchado, Arturo, Maraston, Claudia, Marques-Chaves, Rui, Martinez Valpuesta, Inma, Masters, Karen L., Mathur, Savita, Mcgreer, Ian D., Merloni, Andrea, Merrifield, Michael R., Meszaros, Szabolcs, Meza, Andres, Miglio, Andrea, Minchev, Ivan, Molaverdikhani, Karan, Montero-Dorta, Antonio D., Mosser, Benoit, Muna, Demitri, Myers, Adam, Nair, Preethi, Nandra, Kirpal, Ness, Melissa, Newman, Jeffrey A., Nichol, Robert C., Nidever, David L., Nitschelm, Christian, O Connell, Julia, Oravetz, Audrey, Padilla, Nelson, Palanque-Delabrouille, Nathalie, Pan, Kaike, Parejko, John, Paris, Isabelle, Peacock, John A., Peirani, Sebastien, Pellejero-Ibanez, Marcos, Penny, Samantha, Percival, Will J., Percival, Jeffrey W., Perez-Fournon, Ismael, Petitjean, Patrick, Pieri, Matthew, Pinsonneault, Marc H., Pisani, Alice, Prada, Francisco, Prakash, Abhishek, Price-Jones, Natalie, Raddick, M. Jordan, Rahman, Mubdi, Raichoor, Anand, Barboza Rembold, Sandro, Reyna, A. M., Rich, James, Richstein, Hannah, Ridl, Jethro, Riffel, Rogerio, Riffel, Rogemar A., Rix, Hans-Walter, Robin, Annie C., Rockosi, Constance M., Rodriguez-Torres, Sergio, Rodrigues, Thaise S., Roe, Natalie, Lopes, A. Roman, Roman-Zuniga, Carlos, Ross, Ashley J., Rossi, Graziano, Ruan, John, Ruggeri, Rossana, Runnoe, Jessie C., Salazar-Albornoz, Salvador, Salvato, Mara, Sanchez, Ariel G., Sanchez, Sebastian F., Sanchez-Gallego, Jose R., Santiago, Basilio Xavier, Schiavon, Ricardo, Schimoia, Jaderson S., Schlafly, Eddie, Schlegel, David J., Schneider, Donald P., Schoenrich, Ralph, Schultheis, Mathias, Schwope, Axel, Seo, Hee-Jong, Serenelli, Aldo, Sesar, Branimir, Shao, Zhengyi, Shetrone, Matthew, Shull, Michael, Silva Aguirre, Victor, Skrutskie, M. F., Slosar, Anže, Smith, Michael, Smith, Verne V., Sobeck, Jennifer, Somers, Garrett, Souto, Diogo, Stark, David V., Stassun, Keivan G., Steinmetz, Matthias, Stello, Dennis, Storchi Bergmann, Thaisa, Strauss, Michael A., Streblyanska, Alina, Stringfellow, Guy S., Suarez, Genaro, Sun, Jing, Taghizadeh-Popp, Manuchehr, Tang, Baitian, Tao, Charling, Tayar, Jamie, Tembe, Mita, Thomas, Daniel, Tinker, Jeremy, Tojeiro, Rita, Tremonti, Christy, Troup, Nicholas, Trump, Jonathan R., Unda-Sanzana, Eduardo, Valenzuela, O., Den Bosch, Remco, Vargas-Magana, Mariana, Vazquez, Jose Alberto, Villanova, Sandro, Vivek, M., Vogt, Nicole, Wake, David, Walterbos, Rene, Wang, Yuting, Wang, Enci, Weaver, Benjamin Alan, Weijmans, Anne-Marie, Weinberg, David H., Westfall, Kyle B., Whelan, David G., Wilcots, Eric, Wild, Vivienne, Williams, Rob A., Wilson, John, Wood-Vasey, W. M., Wylezalek, Dominika, Xiao, Ting, Yan, Renbin, Yang, Meng, Ybarra, Jason E., Yeche, Christophe, Yuan, Fang-Ting, Zakamska, Nadia, Zamora, Olga, Zasowski, Gail, Zhang, Kai, Zhao, Cheng, Zhao, Gong-Bo, Zheng, Zheng, Zhou, Zhi-Min, Zhu, Guangtun, Zinn, Joel C., Zou, Hu, Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), and Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC)
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Astrophysics of Galaxies, ComputingMilieux_MISCELLANEOUS
Abstract: The fourth generation of the Sloan Digital Sky Survey (SDSS-IV) began observations in July 2014. It pursues three core programs: APOGEE-2, MaNGA, and eBOSS. In addition, eBOSS contains two major subprograms: TDSS and SPIDERS. This paper describes the first data release from SDSS-IV, Data Release 13 (DR13), which contains new data, reanalysis of existing data sets and, like all SDSS data releases, is inclusive of previously released data. DR13 makes publicly available 1390 spatially resolved integral field unit observations of nearby galaxies from MaNGA, the first data released from this survey. It includes new observations from eBOSS, completing SEQUELS. In addition to targeting galaxies and quasars, SEQUELS also targeted variability-selected objects from TDSS and X-ray selected objects from SPIDERS. DR13 includes new reductions of the SDSS-III BOSS data, improving the spectrophotometric calibration and redshift classification. DR13 releases new reductions of the APOGEE-1 data from SDSS-III, with abundances of elements not previously included and improved stellar parameters for dwarf stars and cooler stars. For the SDSS imaging data, DR13 provides new, more robust and precise photometric calibrations. Several value-added catalogs are being released in tandem with DR13, in particular target catalogs relevant for eBOSS, TDSS, and SPIDERS, and an updated red-clump catalog for APOGEE. This paper describes the location and format of the data now publicly available, as well as providing references to the important technical papers that describe the targeting, observing, and data reduction. The SDSS website, http://www.sdss.org, provides links to the data, tutorials and examples of data access, and extensive documentation of the reduction and analysis procedures. DR13 is the first of a scheduled set that will contain new data and analyses from the planned ~6-year operations of SDSS-IV., Comment: Full information on DR13 available at http://www.sdss.org. Comments welcome to spokesperson@sdss.org. To be published in ApJS

35. The Seventeenth Data Release of the Sloan Digital Sky Surveys: Complete Release of MaNGA, MaStar, and APOGEE-2 Data

Author: null Abdurro’uf, Katherine Accetta, Conny Aerts, Víctor Silva Aguirre, Romina Ahumada, Nikhil Ajgaonkar, N. Filiz Ak, Shadab Alam, Carlos Allende Prieto, Andrés Almeida, Friedrich Anders, Scott F. Anderson, Brett H. Andrews, Borja Anguiano, Erik Aquino-Ortíz, Alfonso Aragón-Salamanca, Maria Argudo-Fernández, Metin Ata, Marie Aubert, Vladimir Avila-Reese, Carles Badenes, Rodolfo H. Barbá, Kat Barger, Jorge K. Barrera-Ballesteros, Rachael L. Beaton, Timothy C. Beers, Francesco Belfiore, Chad F. Bender, Mariangela Bernardi, Matthew A. Bershady, Florian Beutler, Christian Moni Bidin, Jonathan C. Bird, Dmitry Bizyaev, Guillermo A. Blanc, Michael R. Blanton, Nicholas Fraser Boardman, Adam S. Bolton, Médéric Boquien, Jura Borissova, Jo Bovy, W. N. Brandt, Jordan Brown, Joel R. Brownstein, Marcella Brusa, Johannes Buchner, Kevin Bundy, Joseph N. Burchett, Martin Bureau, Adam Burgasser, Tuesday K. Cabang, Stephanie Campbell, Michele Cappellari, Joleen K. Carlberg, Fábio Carneiro Wanderley, Ricardo Carrera, Jennifer Cash, Yan-Ping Chen, Wei-Huai Chen, Brian Cherinka, Cristina Chiappini, Peter Doohyun Choi, S. Drew Chojnowski, Haeun Chung, Nicolas Clerc, Roger E. Cohen, Julia M. Comerford, Johan Comparat, Luiz da Costa, Kevin Covey, Jeffrey D. Crane, Irene Cruz-Gonzalez, Connor Culhane, Katia Cunha, Y. Sophia Dai, Guillermo Damke, Jeremy Darling, James W. Davidson Jr., Roger Davies, Kyle Dawson, Nathan De Lee, Aleksandar M. Diamond-Stanic, Mariana Cano-Díaz, Helena Domínguez Sánchez, John Donor, Chris Duckworth, Tom Dwelly, Daniel J. Eisenstein, Yvonne P. Elsworth, Eric Emsellem, Mike Eracleous, Stephanie Escoffier, Xiaohui Fan, Emily Farr, Shuai Feng, José G. Fernández-Trincado, Diane Feuillet, Andreas Filipp, Sean P Fillingham, Peter M. Frinchaboy, Sebastien Fromenteau, Lluís Galbany, Rafael A. García, D. A. García-Hernández, Junqiang Ge, Doug Geisler, Joseph Gelfand, Tobias Géron, Benjamin J. Gibson, Julian Goddy, Diego Godoy-Rivera, Kathleen Grabowski, Paul J. Green, Michael Greener, Catherine J. Grier, Emily Griffith, Hong Guo, Julien Guy, Massinissa Hadjara, Paul Harding, Sten Hasselquist, Christian R. Hayes, Fred Hearty, Jesús Hernández, Lewis Hill, David W. Hogg, Jon A. Holtzman, Danny Horta, Bau-Ching Hsieh, Chin-Hao Hsu, Yun-Hsin Hsu, Daniel Huber, Marc Huertas-Company, Brian Hutchinson, Ho Seong Hwang, Héctor J. Ibarra-Medel, Jacob Ider Chitham, Gabriele S. Ilha, Julie Imig, Will Jaekle, Tharindu Jayasinghe, Xihan Ji, Jennifer A. Johnson, Amy Jones, Henrik Jönsson, Ivan Katkov, Dr. Arman Khalatyan, Karen Kinemuchi, Shobhit Kisku, Johan H. Knapen, Jean-Paul Kneib, Juna A. Kollmeier, Miranda Kong, Marina Kounkel, Kathryn Kreckel, Dhanesh Krishnarao, Ivan Lacerna, Richard R. Lane, Rachel Langgin, Ramon Lavender, David R. Law, Daniel Lazarz, Henry W. Leung, Ho-Hin Leung, Hannah M. Lewis, Cheng Li, Ran Li, Jianhui Lian, Fu-Heng Liang, Lihwai Lin, Yen-Ting Lin, Sicheng Lin, Chris Lintott, Dan Long, Penélope Longa-Peña, Carlos López-Cobá, Shengdong Lu, Britt F. Lundgren, Yuanze Luo, J. Ted Mackereth, Axel de la Macorra, Suvrath Mahadevan, Steven R. Majewski, Arturo Manchado, Travis Mandeville, Claudia Maraston, Berta Margalef-Bentabol, Thomas Masseron, Karen L. Masters, Savita Mathur, Richard M. McDermid, Myles Mckay, Andrea Merloni, Michael Merrifield, Szabolcs Meszaros, Andrea Miglio, Francesco Di Mille, Dante Minniti, Rebecca Minsley, Antonela Monachesi, Jeongin Moon, Benoit Mosser, John Mulchaey, Demitri Muna, Ricardo R. Muñoz, Adam D. Myers, Natalie Myers, Seshadri Nadathur, Preethi Nair, Kirpal Nandra, Justus Neumann, Jeffrey A. Newman, David L. Nidever, Farnik Nikakhtar, Christian Nitschelm, Julia E. O’Connell, Luis Garma-Oehmichen, Gabriel Luan Souza de Oliveira, Richard Olney, Daniel Oravetz, Mario Ortigoza-Urdaneta, Yeisson Osorio, Justin Otter, Zachary J. Pace, Nelson Padilla, Kaike Pan, Hsi-An Pan, Taniya Parikh, James Parker, Sebastien Peirani, Karla Peña Ramírez, Samantha Penny, Will J. Percival, Ismael Perez-Fournon, Marc Pinsonneault, Frédérick Poidevin, Vijith Jacob Poovelil, Adrian M. Price-Whelan, Anna Bárbara de Andrade Queiroz, M. Jordan Raddick, Amy Ray, Sandro Barboza Rembold, Nicole Riddle, Rogemar A. Riffel, Rogério Riffel, Hans-Walter Rix, Annie C. Robin, Aldo Rodríguez-Puebla, Alexandre Roman-Lopes, Carlos Román-Zúñiga, Benjamin Rose, Ashley J. Ross, Graziano Rossi, Kate H. R. Rubin, Mara Salvato, Sebástian F. Sánchez, José R. Sánchez-Gallego, Robyn Sanderson, Felipe Antonio Santana Rojas, Edgar Sarceno, Regina Sarmiento, Conor Sayres, Elizaveta Sazonova, Adam L. Schaefer, Ricardo Schiavon, David J Schlegel, Donald P. Schneider, Mathias Schultheis, Axel Schwope, Aldo Serenelli, Javier Serna, Zhengyi Shao, Griffin Shapiro, Anubhav Sharma, Yue Shen, Matthew Shetrone, Yiping Shu, Joshua D. Simon, M. F. Skrutskie, Rebecca Smethurst, Verne Smith, Jennifer Sobeck, Taylor Spoo, Dani Sprague, David V. Stark, Keivan G. Stassun, Matthias Steinmetz, Dennis Stello, Alexander Stone-Martinez, Thaisa Storchi-Bergmann, Guy S. Stringfellow, Amelia Stutz, Yung-Chau Su, Manuchehr Taghizadeh-Popp, Michael S. Talbot, Jamie Tayar, Eduardo Telles, Johanna Teske, Ani Thakar, Christopher Theissen, Andrew Tkachenko, Daniel Thomas, Rita Tojeiro, Hector Hernandez Toledo, Nicholas W. Troup, Jonathan R. Trump, James Trussler, Jacqueline Turner, Sarah Tuttle, Eduardo Unda-Sanzana, José Antonio Vázquez-Mata, Marica Valentini, Octavio Valenzuela, Jaime Vargas-González, Mariana Vargas-Magaña, Pablo Vera Alfaro, Sandro Villanova, Fiorenzo Vincenzo, David Wake, Jack T. Warfield, Jessica Diane Washington, Benjamin Alan Weaver, Anne-Marie Weijmans, David H. Weinberg, Achim Weiss, Kyle B. Westfall, Vivienne Wild, Matthew C. Wilde, John C. Wilson, Robert F. Wilson, Mikayla Wilson, Julien Wolf, W. M. Wood-Vasey, Renbin Yan, Olga Zamora, Gail Zasowski, Kai Zhang, Cheng Zhao, Zheng Zheng, Kai Zhu, Institute of Astronomy [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Radboud University [Nijmegen], Department of Physics and Astronomy [Aarhus], Aarhus University [Aarhus], Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Instituto de Astrofisica de Canarias (IAC), Universidad de Antofagasta, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of St Andrews. School of Physics and Astronomy, University of St Andrews. Centre for Contemporary Art, European Space Agency, National Aeronautics and Space Administration (US), Alfred P. Sloan Foundation, and Abdurro'uf, Katherine Accetta, Conny Aerts, Victor Silva Aguirre, Romina Ahumada, Nikhil Ajgaonkar, N. Filiz Ak, Shadab Alam, Carlos Allende Prieto, Andres Almeida, Friedrich Anders, Scott F. Anderson, Brett H. Andrews, Borja Anguiano, Erik Aquino-Ortiz, Alfonso Aragon-Salamanca, Maria Argudo-Fernandez, Metin Ata, Marie Aubert, Vladimir Avila-Reese, Carles Badenes, Rodolfo H. Barba, Kat Barger, Jorge K. Barrera-Ballesteros, Rachael L. Beaton, Timothy C. Beers, Francesco Belfiore, Chad F. Bender, Mariangela Bernardi, Matthew A. Bershady, Florian Beutler, Christian Moni Bidin, Jonathan C. Bird, Dmitry Bizyaev, Guillermo A. Blanc, Michael R. Blanton, Nicholas Fraser Boardman, Adam S. Bolton, Mederic Boquien, Jura Borissova, Jo Bovy, W.N. Brandt, Jordan Brown, Joel R. Brownstein, Marcella Brusa, Johannes Buchner, Kevin Bundy, Joseph N. Burchett, Martin Bureau, Adam Burgasser, Tuesday K. Cabang, Stephanie Campbell, Michele Cappellari, Joleen K. Carlberg, Fabio Carneiro Wanderley, Ricardo Carrera, Jennifer Cash, Yan-Ping Chen, Wei-Huai Chen, Brian Cherinka, Cristina Chiappini, Peter Doohyun Choi, S. Drew Chojnowski, Haeun Chung, Nicolas Clerc, Roger E. Cohen, Julia M. Comerford, Johan Comparat, Luiz da Costa, Kevin Covey, Jeffrey D. Crane, Irene Cruz-Gonzalez, Connor Culhane, Katia Cunha, Y. Sophia Dai, Guillermo Damke, Jeremy Darling, James W. Davidson Jr., Roger Davies, Kyle Dawson, Nathan De Lee, Aleksandar M. Diamond-Stanic, Mariana Cano-Diaz, Helena Dominguez Sanchez, John Donor, Chris Duckworth, Tom Dwelly, Daniel J. Eisenstein, Yvonne P. Elsworth, Eric Emsellem, Mike Eracleous, Stephanie Escoffier, Xiaohui Fan, Emily Farr, Shuai Feng, Jose G. Fernandez-Trincado, Diane Feuillet, Andreas Filipp, Sean P Fillingham, Peter M. Frinchaboy , Sebastien Fromenteau, Lluis Galbany, Rafael A. Garcia, D. A. Garcia-Hernandez, Junqiang Ge, Doug Geisler, Joseph Gelfand, Tobias Geron, Benjamin J. Gibson, Julian Goddy, Diego Godoy-Rivera, Kathleen Grabowski, Paul J. Green, Michael Greener, Catherine J. Grier, Emily Griffith, Hong Guo, Julien Guy, Massinissa Hadjara, Paul Harding, Sten Hasselquist, Christian R. Hayes, Fred Hearty, Jesus Hernandez, Lewis Hill, David W. Hogg, Jon A. Holtzman, Danny Horta, Bau-Ching Hsieh, Chin-Hao Hsu, Yun-Hsin Hsu, Daniel Huber, Marc Huertas-Company, Brian Hutchinson, Ho Seong Hwang, Hector J. Ibarra-Medel, Jacob Ider Chitham, Gabriele S. Ilha, Julie Imig, Will Jaekle, Tharindu Jayasinghe, Xihan Ji, Jennifer A. Johnson, Amy Jones, Henrik Jonsson, Ivan Katkov, Dr. Arman Khalatyan, Karen Kinemuchi, Shobhit Kisku, Johan H. Knapen, Jean-Paul Kneib, Juna A. Kollmeier, Miranda Kong, Marina Kounkel, Kathryn Kreckel, Dhanesh Krishnarao, Ivan Lacerna, Richard R. Lane, Rachel Langgin, Ramon Lavender, David R. Law, Daniel Lazarz, Henry W. Leung, Ho-Hin Leung, Hannah M. Lewis, Cheng Li, Ran Li, Jianhui Lian, Fu-Heng Liang, Lihwai Lin, Yen-Ting Lin, Sicheng Lin, Chris Lintott, Dan Long, Penelope Longa-Pena, Carlos Lopez-Coba, Shengdong Lu, Britt F. Lundgren, Yuanze Luo, J. Ted Mackereth, Axel de la Macorra, Suvrath Mahadevan, Steven R. Majewski, Arturo Manchado, Travis Mandeville, Claudia Maraston, Berta Margalef-Bentabol, Thomas Masseron, Karen L. Masters, Savita Mathur, Richard M. McDermid, Myles Mckay, Andrea Merloni, Michael Merrifield, Szabolcs Meszaros, Andrea Miglio, Francesco Di Mille, Dante Minniti, Rebecca Minsley, Antonela Monachesi, Jeongin Moon, Benoit Mosser, John Mulchaey, Demitri Muna, Ricardo R. Munoz, Adam D. Myers, Natalie Myers, Seshadri Nadathur, Preethi Nair, Kirpal Nandra, Justus Neumann, Jeffrey A. Newman, David L. Nidever, Farnik Nikakhtar, Christian Nitschelm, Julia E. O'Connell, Luis Garma-Oehmichen, Gabriel Luan Souza de Oliveira, Richard Olney, Daniel Oravetz, Mario Ortigoza-Urdaneta, Yeisson Osorio, Justin Otter, Zachary J. Pace, Nelson Padilla, Kaike Pan, Hsi-An Pan, Taniya Parikh, James Parker, Sebastien Peirani, Karla Pena Ramirez, Samantha Penny, Will J. Percival, Ismael Perez-Fournon, Marc Pinsonneault, Frederick Poidevin, Vijith Jacob Poovelil, Adrian M. Price-Whelan, Anna Barbara de Andrade Queiroz, M. Jordan Raddick, Amy Ray, Sandro Barboza Rembold, Nicole Riddle, Rogemar A. Riffel, Rogerio Riffel, Hans-Walter Rix, Annie C. Robin, Aldo Rodriguez-Puebla, Alexandre Roman-Lopes, Carlos Roman-Zuniga, Benjamin Rose, Ashley J. Ross, Graziano Rossi, Kate H. R. Rubin, Mara Salvato, Sebastian F. Sanchez, Jose R. Sanchez-Gallego, Robyn Sanderson, Felipe Antonio Santana Rojas, Edgar Sarceno, Regina Sarmiento, Conor Sayres, Elizaveta Sazonova, Adam L. Schaefer, Ricardo Schiavon, David J Schlegel, Donald P. Schneider, Mathias Schultheis, Axel Schwope, Aldo Serenelli, Javier Serna, Zhengyi Shao, Griffin Shapiro, Anubhav Sharma, Yue Shen, Matthew Shetrone, Yiping Shu, Joshua D. Simon, M. F. Skrutskie, Rebecca Smethurst, Verne Smith, Jennifer Sobeck, Taylor Spoo, Dani Sprague, David V. Stark, Keivan G. Stassun, Matthias Steinmetz, Dennis Stello, Alexander Stone-Martinez, Thaisa Storchi-Bergmann, Guy S. Stringfellow, Amelia Stutz, Yung-Chau Su, Manuchehr Taghizadeh-Popp, Michael S. Talbot, Jamie Tayar, Eduardo Telles, Johanna Teske, Ani Thakar, Christopher Theissen, Daniel Thomas, Andrew Tkachenko, Rita Tojeiro, Hector Hernandez Toledo, Nicholas W. Troup, Jonathan R. Trump, James Trussler, Jacqueline Turner, Sarah Tuttle, Eduardo Unda-Sanzana, Jose Antonio Vazquez-Mata, Marica Valentini, Octavio Valenzuela, Jaime Vargas-Gonzalez, Mariana Vargas-Magana, Pablo Vera Alfaro, Sandro Villanova, Fiorenzo Vincenzo, David Wake, Jack T. Warfield, Jessica Diane Washington, Benjamin Alan Weaver, Anne-Marie Weijmans, David H. Weinberg, Achim Weiss, Kyle B. Westfall, Vivienne Wild, Matthew C. Wilde, John C. Wilson, Robert F. Wilson, Mikayla Wilson, Julien Wolf, W. M. Wood-Vasey, Renbin Yan, Olga Zamora, Gail Zasowski, Kai Zhang, Cheng Zhao, Zheng Zheng, Zheng Zheng, Kai Zhu
Subjects: ABSORPTION-LINE SPECTRA, ACTIVE GALACTIC NUCLEI, anisotropic power spectrum, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics - astrophysics of galaxies, absorption-line spectra, FOS: Physical sciences, Astronomy & Astrophysics, large-scale structure, OSCILLATION SPECTROSCOPIC SURVEY, cluster chemical abundances, reverberation mapping project, Astronomi, astrofysik och kosmologi, LARGE-SCALE STRUCTURE, Astronomy, Astrophysics and Cosmology, QB Astronomy, OLD STELLAR POPULATIONS, CLUSTER CHEMICAL ABUNDANCES, Instrumentation and Methods for Astrophysics (astro-ph.IM), QC, QB, MCC, FINAL TARGETING STRATEGY, Science & Technology, REVERBERATION MAPPING PROJECT, DAS, Astronomy and Astrophysics, ANISOTROPIC POWER SPECTRUM, oscillation spectroscopic survey, Astrophysics - Astrophysics of Galaxies, final targeting strategy, sdss-iv manga, QC Physics, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), active galactic nuclei, Physical Sciences, old stellar populations, Astrophysics - Instrumentation and Methods for Astrophysics, SDSS-IV MANGA, Astrophysics - instrumentation and methods for Astrophysics
Abstract: Abdurro’uf et al., This paper documents the seventeenth data release (DR17) from the Sloan Digital Sky Surveys; the fifth and final release from the fourth phase (SDSS-IV). DR17 contains the complete release of the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey, which reached its goal of surveying over 10,000 nearby galaxies. The complete release of the MaNGA Stellar Library accompanies this data, providing observations of almost 30,000 stars through the MaNGA instrument during bright time. DR17 also contains the complete release of the Apache Point Observatory Galactic Evolution Experiment 2 survey that publicly releases infrared spectra of over 650,000 stars. The main sample from the Extended Baryon Oscillation Spectroscopic Survey (eBOSS), as well as the subsurvey Time Domain Spectroscopic Survey data were fully released in DR16. New single-fiber optical spectroscopy released in DR17 is from the SPectroscipic IDentification of ERosita Survey subsurvey and the eBOSS-RM program. Along with the primary data sets, DR17 includes 25 new or updated value-added catalogs. This paper concludes the release of SDSS-IV survey data. SDSS continues into its fifth phase with observations already underway for the Milky Way Mapper, Local Volume Mapper, and Black Hole Mapper surveys., This publication uses data generated via the Zooniverse.org platform, development of which is funded by generous support, including a Global Impact Award from Google, and by a grant from the Alfred P. Sloan Foundation. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.
Published: 2022
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35 results on '"Lin, Yen Ting"'

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