Academia Sinica Institute of Astronomy & Astrophysics
中央研究院天文及天文物理研究所
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Cosmology

Measurement of the acoustic peaks of the full-sky cosmic microwave background (CMB) temperature anisotropies has been instrumental in deciding the geometry and content of the universe, e.g. the first acoustic peak at ell~220 indicating a flat universe. However, acoustic peak positions vary in different parts of the sky due to statistical fluctuation. We test the statistics of the peak positions of small patches from ESA Planck data. By defining the "distance": how far the first 3 peaks positions are away from those in the best-fit LambdaCDM model, we found the patch (left) containing the mysterious "Cold Spot", an area near the Eridanus constellation where the temperature is significantly (p~0.01) lower than Gaussian theory predicts, displays large synchronous shift of peak positions towards smaller multipole numbers with significance lower than 1.11x10^{-4} ( right: the power spectrum of that patch from 4 different Planck CMB maps). The combination of large synchronous shifts in acoustic peaks and lower than usual temperature at the Cold Spot area results in a 4.73 sigma detection. We thus propose there is some extra localized unknown energy to stretch out the space in the transverse direction around the Cold Spot area to simultaneously account for the Cold Spot, excessive shift of the acoustic peaks, and the large under-dense regions.
Excessive shift of the CMB acoustic peaks of the Cold Spot area
Cosmological simulations suggest that the first stars were very massive. They could emit a large amount of UV radiation and create extensive HII regions.
The HII region around the first star
Metallicity distribution after the first supernova explosion. The metal-rich ejecta has been dispersed to ~ 1 kpc and polluted the pristine IGM gas at 20 Myr after the explosion.
Chemical Enrichment of the First Supernovae
Estimation of the effective inflight beam of WMAP Q1 Differencing Assembly in Ecliptic Coordinate. The bar denotes the asymmetry R= r_maj /r_min -1, where r_maj and r_min are the major and minor axis of the elliptical shape of the beam, respectively, and the orientation of the major axis is denoted by that of the bar.
Estimated beam of WMAP Q1 Differencing Assembly Map in Ecliptic Coordinate
Posterior probability distribution function of H0, Ωde, w, and Ωk for supernovae (SN; turquoise dot-dashed; Hicken et al. 2009), baryon acoustic oscillation (BAO; magenta dashed; Percival et al. 2010), time-delay lenses (black solid; Suyu et al. 2013) when each is combined with WMAP7 (Komatsu et al. 2011) assuming a non-flat wCDM cosmology with a time-independent dark energy equation of state. Contours mark the 68%, and 95% credible regions. Time-delay lenses are highly complementary to other probes, particularly the cosmic microwave background and SN.
Cosmological constraints from gravitational lens time delays
Histogram of the estimated beam orientation of WMAP Internal Linear Combination Map in Ecliptic Coordinate. The angle is defined with that between the bar and the Ecliptic Equator.
Histogram of the estimated beam orientation of WMAP Internal Linear Combination Map in Ecliptic Coordinate
The histogram of the estimated beam asymmetry R= r_maj /r_min -1 of WMAP Internal Linear Combination Map, where r_maj and r_min are the major and minor axis of the elliptical shape of the beam, respectively.
Histogram of the estimated beam asymmetry of WMAP Internal Linear Combination Map
Estimation of the effective inflight beam of WMAP Internal Linear Combination in Ecliptic Coordinate. The bar denotes the asymmetry R= r_maj /r_min -1, where r_maj and r_min are the major and minor axis of the elliptical shape of the beam, respectively, and the orientation of the major axis is denoted by that of the bar.
Estimated beam of WMAP Internal Linear Combination Map in Ecliptic Coordinate
Histogram of the estimated beam orientation of WMAP Q1 Differencing Assembly Map in Ecliptic Coordinate. The angle is defined with that between the major axis and the Ecliptic Equator.
Histogram of the estimated beam orientation of WMAP Q1 Differencing Assembly Map in Ecliptic Coordinate
The histogram of the estimated beam asymmetry R= r_maj /r_min -1 of WMAP Q1 Differencing Assembly Map, where r_maj and r_min are the major and minor axis of the elliptical shape of the beam, respectively.
Histogram of the estimated beam asymmetry of WMAP Q1 Differencing Assembly Map
Image of the gravitational lens RXJ1131−1231, taken with the Advanced Camera for Surveys on the Hubble Space Telescope. The lensed AGN images of the spiral source galaxy are marked by A, B, C, and D, and the star forming regions of the spiral galaxy form the spectacular lensed structures. The primary and satellite lens galaxies are indicated by G and S, respectively. The cosmological time-delay distance to the lens, which is primarily sensitive to the Hubble constant, can be measured by obtaining the time delays between the multiple images and modeling the mass distributions of the lens galaxies and line-of-sight structures.
Strong gravitational lens system with time delays
Near-infrared K-band (2.2 micron) luminosity density as a function of comoving distance in the local universe. Data points show measurements from this study and others from the literature. The right hand vertical axis shows total matter density contrast assuming K-band luminosity density is an unbiased tracer of mass density. The curved lines show radial density profiles from two models that invoke a local under-density to fit the type Ia supernovae data without dark energy. The "step function" shows another model that uses a local under-density to reconcile the discrepancy between local measurements of the Hubble constant and those inferred by Planck.
Evidence for a 300 Mpc Radius Local Under-density
Subaru BVRIz composite color images centered on the galaxy cluster MACS1206 (z=0.439), overlaid with mass contours from our joint strong-and-weak lensing analysis of HST and Subaru observations. The image size in the left panel is 24 arcminutes (~8Mpc) on a side. The cluster is fairly centrally concentrated in projection, and associated with elongated large scale structure running north-east south-east, both in the projected mass and galaxy distributions.
Mass Distribution in and around the Galaxy Cluster MACS J1206.2-0847
Three-dimensional cross power spectrum of the 21cm emission measured at the Green Bank Telescope and the optical density field traced by the WiggleZ redshift survey. Negative points are shown with reversed sign and a thin line. The solid line is the mean of simulations based on the empirical non-linear model of Blake et al. (2011) processed by the same pipeline. The overall amplitude is consistent with a measurement of Omega_HI~4*10^(-4) at z=0.8, similar to the value measured at z=0.
21cm brightness fluctuation at z=0.8 in cross-correlation
Direct measurement of the CMB angular power spectrum. From WMAP V band map we choose patches with σ < 98 μK (after eliminating bright point sources), and we take the cross-power spectra of patches between WMAP V and W band. After deconvolution of the window functions, the power spectra of the 47 patches are shown in black dot and the mean power spectrum is in big blue dot. For comparison we plot in big orange dot the power spectrum binned (⊿l = 15) from that by the WMAP science team. The best-fit CDM model is in solid line.
Direct measurement of the angular power spectrum of cosmic microwave background temperature anisotropies in the WMAP Data
A cross-correlation measurement of 21-cm emission measured by the Green Bank Telescope, and the optical galaxies measured by the DEEP2 galaxy survey.
An intensity map of hydrogen 21-cm emission at redshift z ≈ 0.8
Average power spectrum in units of K 2 of all combinations of days, excluding December 11, as a function of the multipole moment l. Each point is shown with a 2σ upper limit derived from a bootstrap error analysis, which is in most cases smaller than the size of the point. The points are logarithmically spaced as described in the text, from left to right covering the ranges 377 < l < 578, 578 < l < 899 and 899 < l < 1414. Triangles are the power before subtracting foregrounds, diamonds are after 8 MHz mean subtraction, squares are after 2 MHz mean subtraction and circles are after 0.5 MHz subtraction. The curved solid line is the theoretical EoR signal from Jelic et al. (2008), and the dashed line is the theoretical EoR signal ´ with a cold absorbing IGM as described in the text.
The GMRT Epoch of Reionization experiment: a new upper limit on the neutral hydrogen power spectrum at z ≈ 8.6
Model-free direct reconstruction of full mass profiles for five massive galaxy clusters, A1689, A1703, A370, Cl0024+17, and RXJ1347-11, from combined weak and strong gravitational lensing.
Full mass profiles of five massive galaxy clusters
The figure represents the three-dimensional galaxy distribution for about 1/10 field of view of the RCS photometric redshift catalog (Hsieh et al. 2005, ApJS, 158, 161; Gladders and Yee 2005, ApJS, 157, 1) with the Earth at the origin. Each red dot indicate
Three-dimensional galaxy distribution for about 1/10 field of view of the RCS photometric redshift catalog
A Subaru Suprime-Cam image of one of the clusters used in the analysis, A2390, (2.7 billion light years from the Earth). The purple hue shows the dark matter distribution measured by the gravitational lensing effect on distant galaxies (typically 8 billion light years from the Earth), where the darker color indicates the denser dark matter concentration. It shows that the dark matter distribution is elongated along the northwest-southeast direction.
Direct measurement of dark matter halo ellipticity of massive clusters

Cosmology is the study of the large-scale properties of the universe as a whole. Our goal in cosmological studies is to understand the nature, origin, and evolution of the whole universe. The universe is the sum of all matter and energies, space and time, and the laws of nature. Cosmology involves the formation of theoretical models to describe our universe, which then provide us with specific predictions for physical phenomena that can be tested with astronomical experiments.

The research of the cosmology group at IAA has been focusing on the measurement analysis of the cosmic microwave background (CMB) and using multiwavelength observation and analysis on galaxy formation at high redshift and galaxy clusters in order to understand their properties and place constraints on the properties of dark energy (DE) and dark matter (DM).

Research Members (17)

Wang, Wei-Hao 王為豪 cv Deputy Director; Research Fellow
Research Interest: Multiwavelength observational studies of galaxy formation and evolution at high redshift
Koch, Patrick 高培邁 cv Research Fellow
Research Interest: Structure Formation, Star and Planet Formation, Clusters of Galaxies, Analysis Techniques, Telescope Commissioning
Lin, Li-Hwai 林俐暉 cv Research Fellow
Research Interest: Galaxy Evolution; Interacting Galaxies; Galaxy Clusters; Optical/Infrared Astronomy
Lin, Yen-Ting 林彥廷 cv Research Fellow
Research Interest: cosmological models constrained by cluster mass function
Okumura, Teppei 奧村哲平 cv Research Fellow
Research Interest: Observational cosmology, Large-scale structure of the Universe, Analysis of large data set and simulations, Galaxy redshift surveys, Gravitational lensing, Dark matter and Dark energy, Modified gravity theory
Umetsu, Keiichi 梅津敬一 cv Research Fellow
Research Interest: Observational Cosmology, Gravitational Lensing, Galaxy Clusters, Large Scale Structure in the Universe
Chen, Chian-Chou 陳建州 cv Assistant Research Fellow
Research Interest: Observational cosmology; Galaxy formation and evolution; Dusty galaxy; OIR/FIR/Submm astrophysics
Chen, Ke-Jung 陳科榮 cv Assistant Research Fellow
Research Interest: Theoretical and Computational Astrophysics: Supernovae of Massive Stars, Inter-Stellar Medium, Supermassive Black Holes, The First Stars and Galaxies
Ng, Kin-Wang 吳建宏 cv Joint Research Fellow; Inst. of Physics, AS
Research Interest: Cosmology & Particle Astrophysics
Chang, Tzu-Ching 張慈錦 cv Visiting Scholar (JPL, Caltech)
Research Interest: 21-cm Cosmology; Cosmic Reionization; Gravitational Lensing; Large-scale Structure
Molnar, Sandor 麥善德 cv Visiting Scholar
Research Interest: Cosmology, Clusters of Galaxies, SZ, X-ray Observations, Numerical Simulations
Suyu, Sherry 蘇游瑄 cv Visiting Scholar(Max Planck Institute for Astrophysics)
Research Interest: Observational cosmology, Galaxy formation and evolution, Dark matter halos of galaxies, Gravitational lensing, Bayesian data analysis methods
Hsieh, Bau-Ching 謝寶慶 cv SuMire Project Research Manager
Research Interest: High-z Galaxies, Large Scale Structure, Galaxy and Galaxy Cluster, Near Infrared/ Optical Astronomy
Lin, Kai-Yang 林凱揚 cv Research Support Staff
Research Interest: Observational Cosmology, Galaxy Cluster; Radio Interferometry
Huang, Chih-Wei Locutus 黃智威 cv GLT/VLBI Support Scientist
Research Interest: Cosmic Microwave Background, Galaxy Clusters, Observational Cosmology
Yan, Chi-Hung 顏吉鴻 cv OIR/EPO Support Engineer
Research Interest: OIR Image Pipeline, Radio Astronomy
Bower, Geoffrey 包傑夫 cv RCUH Research Fellow / ASIAA Research Scientist
Research Interest: Transient radio sources, black holes, radio cosmology, VLBI, radio instrumentation and techniques.

Journal Papers (612)

  1. Chen K-J; Tang C-Y; Whalen DJ; Ho M-Y; Tsai S-H; Ou P-S; Ono M, "How Population III Supernovae Determined the Properties of the First Galaxies" , ApJ: 964(1), id.91 (12pp), Mar, 2024 [SCI] ( ADS | Fulltext )
  2. Hsu Q-N; Cowie LL; Chen C-C; Barger AJ, "A Full Resolution of the 450 μm Extragalactic Background Light" , ApJ: 964(2), L32 (7pp), Apr, 2024 [SCI] ( ADS | Fulltext )
  3. Tang C-Y; Chen K-J, "Clumpy Structures within the Turbulent Primordial Cloud" , MNRAS: 529(4), 4248-4261, Mar, 2024 [SCI] ( ADS | Fulltext )
  4. Lin C-H; Chen K-J; Hwang C-Y, "Rapid Growth of Galactic Supermassive Black Holes through Accreting Giant Molecular Clouds during Major Mergers of their Host Galaxies" , ApJ: 952(2), id.121 (13 pp), Aug, 2023 [SCI] ( ADS | Fulltext )
  5. Okumura T; Taruya A, "First Constraints on Growth Rate from Redshift-space Ellipticity Correlations of SDSS Galaxies at 0.16 < z < 0.70" , ApJL: 945(2), L30 (7pp), March, 2023 [SCI] ( ADS | Fulltext )
  6. Tam S-I; Umetsu K; Robertson A; McCarthy IG, "Testing the Collisionless Nature of Dark Matter with the Radial Acceleration Relation in Galaxy Clusters" , ApJ: 953(2), id.169 (19pp), Aug, 2023 [SCI] ( ADS | Fulltext )
  7. Tsai S-H; Chen K-J; Whalen D; Ou P-S; Woods TE, "The Evolution of Population III and Extremely Metal-Poor Binary Stars" , ApJ: 951(2), id.84, July, 2023 [SCI] ( ADS | Fulltext )
  8. Chiu I-N; Ghirardini V; Liu A; Grandis S; Bulbul E; Bahar YE; Comparat J; Bocquet S; Clerc N; Klein M; Liu T; Li X; Miyatake H; Mohr J; Oguri M; Okabe N; Pacaud F; Ramos-Ceja ME; Reiprich TH; Schrabback T; Umetsu K, "The eROSITA Final Equatorial-Depth Survey (eFEDS). X-ray observable-to-mass-and-redshift relations of galaxy clusters and groups with weak-lensing mass calibration from the Hyper Suprime-Cam Subaru Strategic Program survey" , A&A: 661, id.A11 (41pp), May, 2022 [SCI] ( ADS | Fulltext )
  9. Chuang Y-T; Okumura T; Shirasaki M, "Distinguishing between ΛCDM and f(R) gravity models using halo ellipticity correlations in simulations" , MNRAS: 515(3), 4464-4470, Sep, 2022 [SCI] ( ADS | Fulltext )
  10. Díaz-García LA; Umetsu K; Rasia E; Cui W; Meneghetti M, "The Three Hundred project: dissecting the Fundamental Plane of galaxy clusters up to z = 1" , MNRAS: 512(1), 1214-1233, May, 2022 [SCI] ( ADS | Fulltext )
  11. Tam S-I; Umetsu K; Amara A, "Likelihood-free Forward Modeling for Cluster Weak Lensing and Cosmology" , ApJ: 925(2), id.145 (14pp), Feb, 2022 [SCI] ( ADS | Fulltext )
  12. Umetsu K; Ueda S; Hsieh B-C; Nonino M; Chiu IN; Oguri M; Molnar SM; Koekemoer AM; Tam S-I, "Line-of-sight Elongation and Hydrostatic Mass Bias of the Frontier Fields Galaxy Cluster Abell 370" , ApJ: 934(2), id.169, Aug, 2022 [SCI] ( ADS | Fulltext )
  13. Ng K-W; Wu Y-P, "Constant-rate inflation: primordial black holes from conformal weight transitions" , Journal of High Energy Physics: 2021 (11), id.76, Nov, 2021 [SCI] ( ADS | Fulltext )
  14. Okumura T; Hayashi M; Chiu I-N; Lin Y-T; Osato K; Hsieh B-C; Lin S-C, "Angular clustering and host halo properties of [OII] emitters at z>1 in the Subaru HSC survey" , PASJ: 73(4), 1186-1207, Aug, 2021 [SCI] ( ADS | Fulltext )
  15. Agrawal A; Okumura T; Futamase T, "Standard candles and sirens rescue H0" , ApJ: 904(2), id.169 (6pp), Dec, 2020 [SCI] ( ADS | Fulltext )
  16. Chiu I-N; Okumura T; Oguri M; Agrawal A, ...; Umetsu K; Lin Y-T, "A clustering-based self-calibration of the richness-to-mass relation of CAMIRA galaxy clusters out to z ≍ 1.1 in the Hyper Suprime-Cam survey" , MNRAS: 498(2), 2030-2053, Oct, 2020 [SCI] ( ADS | Fulltext )
  17. Chiu IN; Umetsu K; Murata R; et al., "The Richness-to-Mass Relation of CAMIRA Galaxy Clusters from Weak-lensing Magnification in the Subaru Hyper Suprime-Cam Survey" , MNRAS: 495(1), 428-450, Apr, 2020 [SCI] ( ADS | Fulltext )
  18. Hirashita H; Lin C-Y, "Dust abundance and grain size in galaxy halos" , Planet Space Sci: 183, id.104504 (11pp.), Apr, 2020 [SCI] ( ADS | Fulltext )
  19. Lim C-F; Chen C-C; Smail I; Wang W-H; Tee W-L; Lin Y-T; ...; Toba Y; Chang Y-Y; ...; Simpson JM, "SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES). IV. Spatial Clustering and Halo Masses of Submillimeter Galaxies" , ApJ: 895(2), id.104 (18pp.), Jun, 2020 [SCI] ( ADS | Fulltext )
  20. Molnar SM; Godfrey J, "Empirical Test for Relativistic Kinetic Theories Based on the Sunyaev-Zel'dovich Effect" , ApJ: 902(2), id.143 (12pp.), Oct, 2020 [SCI] ( ADS | Fulltext )
  21. Molnar SM; Ueda S; Umetsu K; et al., "The Dynamical State of the Frontier Fields Galaxy Cluster Abell 370" , ApJ: 900(2), id.151 (10pp.), Sep, 2020 [SCI] ( ADS | Fulltext )
  22. Okumura T; Taruya A, "Anisotropies of galaxy ellipticity correlations in real and redshift space: Angular dependence in linear tidal alignment model" , MNRAS: 493(1), L124-128 (5 pp.), Mar, 2020 [SCI] ( ADS | Fulltext )
  23. Okumura T; Taruya A; Nishimichi T, "Testing tidal alignment models for anisotropic correlations of halo ellipticities with N-body simulations" , MNRAS: 494(1), 694-702 (9pp.), May, 2020 [SCI] ( ADS | Fulltext )
  24. Suyu SH; Huber S; Cañameras R; et al., "HOLISMOKES. I. Highly Optimised Lensing Investigations of Supernovae, Microlensing Objects, and Kinematics of Ellipticals and Spirals" , A&A: 644, id.A162 (15 pp.), Dec, 2020 [SCI] ( ADS | Fulltext )
  25. Umetsu K, "Cluster-Galaxy Weak Lensing" , A&ARv: 28(1), id.7 (101pp.), Dec, 2020 [SCI] ( ADS | Fulltext )
  26. Umetsu K; Sereno M; Lieu M; ...; Chiu IN; Coupon J; ...; Higuchi Y; et al., "Weak-lensing Analysis of X-Ray-selected XXL Galaxy Groups and Clusters with Subaru HSC Data" , ApJ: 890(2), id.148 (36pp.), Feb, 2020 [SCI] ( ADS | Fulltext )
  27. Agrawal A; Okumura T; Futamase T, "Constraining neutrino mass and dark energy with peculiar velocities and lensing dispersions of Type Ia supernovae" , Phys Rev D: 100(6), id. 063534 (8 pp.), Sep, 2019 [SCI] ( ADS | Fulltext )
  28. Aoyama S; Hirashita H; Lim C-F; Chang YY; Wang W-H; et al., "Comparison of cosmological simulations and deep submillimetre galaxy surveys" , MNRAS: 484(2), 1852-1864, Apr, 2019 [SCI] ( ADS | Fulltext )
  29. Hou K-C; Aoyama S; Hirashita H; et al., "Dust scaling relations in a cosmological simulation" , MNRAS: 485(2), 1727-1744, May, 2019 [SCI] ( ADS | Fulltext )
  30. Hsu L-T; Lin L; Dickinson M; ...; Hsieh BC; Wang WH; ...; Yan CH; ...; Wang SY, "Near-Infrared Survey and Photometric Redshifts in the Extended GOODS-North Field" , ApJ: 871(2), 233 (14 pp.), Feb, 2019 [SCI] ( ADS | Fulltext )
  31. Okumura T; Taruya A; Nishimichi T, "Intrinsic alignment statistics of density and velocity fields at large scales: Formulation, modeling, and baryon acoustic oscillation features" , Phys Rev D: 100(10), id. 103507 (22 pp.), Nov, 2019 [SCI] ( ADS | Fulltext )
  32. Aoyama S; Hou K-C; Hirashita H; et al., "Cosmological simulation with dust formation and destruction" , MNRAS: 478(4), 4905-4921, Aug, 2018 [SCI] ( ADS | Fulltext )
  33. Chiang LY, "Excessive shift of the CMB acoustic peaks of the Cold Spot area" , ApJ: 861(1), id. 8 (8 pp.), July, 2018 [SCI] ( ADS | Fulltext )
  34. Chiu I; Mohr JJ; McDonald M; et al., "Baryon Content in a Sample of 91 Galaxy Clusters Selected by the South Pole Telescope at 0.2 < z < 1.25" , MNRAS: 478(3), 3072-3099, Aug, 2018 [SCI] ( ADS | Fulltext )
  35. Chiu IN; Umetsu K; Sereno M; et al., "CLUMP-3D: Three-dimensional Shape and Structure of 20 CLASH Galaxy Clusters from Combined Weak and Strong Lensing" , ApJ: 860(2), id. 126 (23 pp.), June, 2018 [SCI] ( ADS | Fulltext )
  36. Molnar SM; Broadhurst T, "Multi-phenomena Modeling of the New Bullet-like Cluster ZwCl 008.8+52 Using N-body/Hydrodynamical Simulations" , ApJ: 862(2), id. 112 (11 pp.), Aug, 2018 [SCI] ( ADS | Fulltext )
  37. Okumura T; Nishimichi T; Umetsu K; et al., "Splashback radius of nonspherical dark matter halos from cosmic density and velocity fields" , Phys Rev D: 98(2), id. 023523 (18 pp.), July, 2018 [SCI] ( ADS | Fulltext )
  38. Suyu SH; Chang T-C; Courbin F; Okumura T, "Cosmological distance indicators" , Space Sci Rev: 214(5), id. 91 (34 pp.), Aug, 2018 [SCI] ( ADS | Fulltext )
  39. Umetsu K; Sereno M; Tam S-L; Chiu I-N; ...; Okumura T; ...; Higuchi Y; et al., "The Projected Dark and Baryonic Ellipsoidal Structure of 20 CLASH Galaxy Clusters" , ApJ: 806(2), id. 104 (26 pp.), June, 2018 [SCI] ( ADS | Fulltext )
  40. Chang Y-Y; Le Floc'h E; Juneau S; ...; Toba Y; Lim C-F; Tang J-J; Wang W-H; et al., "Infrared Selection of Obscured Active Galactic Nuclei in the COSMOS Field" , ApJS: 233(2), 19-37, Dec, 2017 [SCI] ( ADS | Fulltext )
  41. Molnar SM; Broadhurst T, "Shocks and Tides Quantified in the “Sausage” Cluster, CIZA J2242.8+5301 Using N-body/Hydrodynamical Simulations" , ApJ: 841(1), 46, May 20, 2017 [SCI] ( ADS | Fulltext )
  42. Okumura T; Takada M; More S; et al., "Reconstruction of halo power spectrum from redshift-space galaxy distribution: cylinder-grouping method and halo exclusion effect" , MNRAS: 469(1), 459-475, July, 2017 [SCI] ( ADS | Fulltext )
  43. Simpson J; Smail I; Wang W-H; ...; Lim C-F; Tee W-L; Toba Y; et al., "An Imperfectly Passive Nature: Bright Submillimeter Emission from Dust-obscured Star Formation in the z = 3.717 “Passive” System, ZF 20115" , ApJL: 844(1), L10 ((5 pp.), July, 2017 [SCI] ( ADS | Fulltext )
  44. Suyu SH; Bonvin V; Courbin F; ...; Wong KC; ...; Chen GCF; et al., "H0LiCOW - I. H0 Lenses in COSMOGRAIL's Wellspring: program overview" , MNRAS: 468(3), 2590-2604, July, 2017 [SCI] ( ADS | Fulltext )
  45. Toba Y; Komugi S; Nagao T; Yamashita T; Wang W-H; Imanishi M; Sun A-L, "No sign of strong molecular gas outflow in an infrared-bright dust-obscured galaxy with strong ionized-gas outflow" , ApJ: 851(2), 98-104, Dec 20, 2017 [SCI] ( ADS | Fulltext )
  46. Toba Y; Bae H-J; Nagao T; ...; Wang W-H; ...; Sun A-L; Chang Y-Y, "Ionized gas outflows in infrared-bright dust-obscured galaxies selected with WISE and SDSS" , ApJ: 850(2), 140-155, Dec, 2017 [SCI] ( ADS | Fulltext )
  47. Toba Y; Nagao T; Kajisawa M; ...; Wang W-H;... et al., "Clustering of infrared-bright dust-obscured galaxies revealed by the Hyper Suprime-Cam and WISE" , ApJ: 835(1), 36, Jan, 2017 [SCI] ( ADS | Fulltext )
  48. Umetsu K; Diemer B, "Lensing Constraints on the Mass Profile Shape and the Splashback Radius of Galaxy Clusters" , ApJ: 836(2), 231, Feb, 2017 [SCI] ( ADS | Fulltext )
  49. Wang W-H; Lin W-C; Lim C-F; ...; Chang Y-Y; ...; Simpson J; Tee, W-L; Toba Y; et al., "SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES): Faint-End Counts at 450 um" , ApJ: 850(1), 37, Nov, 2017 [SCI] ( ADS | Fulltext )
  50. Wong KC; Raney C; Keeton CR; Umetsu K; et al., "Joint Strong and Weak Lensing Analysis of the Massive Cluster Field J0850+3604" , ApJ: 844(2), 127, Aug 1, 2017 [SCI] ( ADS | Fulltext )
  51. Wong KC; Suyu SH; Auger MW; et al., "H0LiCOW - IV. Lens mass model of HE 0435-1223 and blind measurement of its time-delay distance for cosmology" , MNRAS: 465(4), 4895-4913, March, 2017 [SCI] ( ADS | Fulltext )
  52. Chan JHH; Suyu SH; More A; ...; Chiueh T; ...; Hsieh B-C; ...; Wang SY, "Galaxy-Scale Gravitational Lens Candidates from the Hyper Suprime-Cam Imaging Survey and the Galaxy and Mass Assembly Spectroscopic Survey" , ApJ: 832(2), 135, Dec, 2016 [SCI] ( ADS | Fulltext )
  53. Chen GC-F; Suyu SH; Wong KC; et al., "SHARP - III. First use of adaptive-optics imaging to constrain cosmology with gravitational lens time delays" , MNRAS: 462(4), 3457-3475, Nov, 2016 [SCI] ( ADS | Fulltext )
  54. Cheng Y-T; Chang T-C; Bock J; et al., "Spectral Line De-confusion in an Intensity Mapping Survey" , ApJ: 832(2), 165, Dec, 2016 [SCI] ( ADS | Fulltext )
  55. Hirashita H; Koch PM; Matsushita S; Takakuwa S; Nakamura M; Asada K; Liu HB; Urata U; Wang M-J; Wang W-H; Takahashi S; Tang Y-W; Chang H-H; Huang K; Morata O; Otsuka M; Lin K-Y; Tsai A-L; Lin Y-T; Srinivasan S; Martin-Cocher P; Pu J-Y; Kemper F; Patel N; Grimes P; Huang Y-D; Han C-C; Huang Y-R; Nishioka H; Lin C-CL; Zhang Q; Keto E; Burgos R; Chen M-T; Inoue M; Ho PTP, "First-generation Science Cases for Ground-based Terahertz Telescopes" , PASJ: 68(1), R1, Feb, 2016 [SCI] ( ADS | Fulltext )
  56. Lin K-Y; Nishioka H; Wang F-C; Huang C-W L; Liao Y-W; Wu J-H P; Koch PM; Umetsu K; Chen MT; ...; Chang S-H; Hoang Ngoc Duy; Han C-C; ...; Ho PTP; Huang Y-D; Jiang H; Li C-T;...; Martin-Cocher P; Molnar SM; et al., "AMiBA: Cluster Sunyaev-Zel'dovich Effect Observations with the Expanded 13-Element Array" , ApJ: 830(2), 91, Oct, 2016 [SCI] ( ADS | Fulltext )
  57. Lin L; Capak P; Laigle C; ...; Hsieh B-C; Jian H-Y; et al., "The SPLASH survey: Quiescent galaxies are more strongly clustered but are not necessarily located in high-density environments" , ApJ: 817(2), 97, Feb, 2016 [SCI] ( ADS | Fulltext )
  58. Molnar SM, "Cluster Physics with Merging Galaxy Clusters" , Frontiers in Astronomy and Space Sciences: 2, id. 7 (31 pp.), Feb, 2016 ( ADS | Fulltext )
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  60. Umetsu K; Zitrin A; Gruen D; et al., "CLASH: Joint Analysis of Strong-lensing, Weak-lensing Shear, and Magnification Data for 20 Galaxy Clusters" , ApJ: 821(2), 116, April 20, 2016 [SCI] ( ADS | Fulltext )
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