MC²: MAPPING THE DARK MATTER DISTRIBUTION OF THE “TOOTHBRUSH” CLUSTER RX J0603.3+4214 WITH<i>HUBBLE SPACE TELESCOPE</i>AND SUBARU WEAK LENSING

Jee, M. James,Dawson, William A.,Stroe, Andra,Wittman, David,van Weeren, Reinout J.,Brü,ggen, Marcus,Bradač,, Maruš,a,Rö,ttgering, Huub American Astronomical Society 2016 The Astrophysical journal Vol.817 No.2

<P>The galaxy cluster RX J0603.3+4214. at z-0.225 is one of the rarest clusters boasting an extremely large (similar to 2 Mpc) radio. relic. Because of the remarkable morphology of the relic, the cluster is nicknamed the. 'Toothbrush Cluster.' Although the cluster's underlying mass distribution is one of the critical pieces of information needed to reconstruct the merger scenario responsible for the puzzling radio. relic morphology, its proximity to the Galactic plane b similar to 10 degrees has imposed significant observational challenges. We present a high-resolution weak-lensing study of the cluster with Subaru/Suprime Cam and Hubble Space Telescope imaging data. Our mass reconstruction reveals that the cluster is composed of complicated dark matter substructures closely tracing the galaxy distribution, in contrast, however, with the relatively simple binary X-ray morphology. Nevertheless, we find that the cluster mass is still dominated by the two most massive clumps aligned north-south with a similar to 3: 1 mass ratio (M-200 = 6.29(-1.62)(+2.24) x 10(14) M-circle dot and 1.98(-0.74)(+1.24) x 10(14) M-circle dot for the northern and southern clumps, respectively). The southern mass peak is similar to 2' offset toward the south with respect to the corresponding X-ray peak, which has a 'bullet'-like morphology pointing south. Comparison of the current weak-lensing result with the X-ray, galaxy, and radio. relic suggests that perhaps the dominant mechanism responsible for the observed relic may be a highspeed collision of the two most massive subclusters, although the peculiarity of the morphology necessitates involvement of additional subclusters. Careful numerical simulations should follow in order to obtain more complete understanding of the merger scenario utilizing all existing observations.</P>

MC²: Subaru and<i>Hubble Space Telescope</i>Weak-lensing Analysis of the Double Radio Relic Galaxy Cluster PLCK G287.0+32.9

Finner, Kyle,Jee, M. James,Golovich, Nathan,Wittman, David,Dawson, William,Gruen, Daniel,Koekemoer, Anton M.,Lemaux, Brian C.,Seitz, Stella American Astronomical Society 2017 The Astrophysical journal Vol.851 No.1

<P>The second most significant detection of the Planck Sunyaev-Zel'dovich survey, PLCK G287.0+32.9 (z = 0.385), boasts two similarly bright radio relics and a radio halo. One radio relic is located similar to 400 kpc NW of the X-ray peak and the other similar to 2.8 Mpc to the SE. This large difference suggests that a complex merging scenario is required. A key missing puzzle for the merging scenario reconstruction is the underlying dark matter distribution in high resolution. We present a joint Subaru Telescope and Hubble Space Telescope weak-lensing analysis of the cluster. Our analysis shows that the mass distribution features four significant substructures. Of the substructures, a primary cluster of mass M-200c = 1.59(-0.22)(+0.25) x 10(15) h(70)(-1) M-circle dot dominates the weak-lensing signal. This cluster is likely to be undergoing a merger with one (or more) subcluster whose mass is approximately a factor of 10 lower. One candidate is the subcluster of mass M-200c = 1.16(-0.13)(+0.15) x 10(14) h(70)(-1) M-circle dot located similar to 400 kpc to the SE. The location of this subcluster suggests that its interaction with the primary cluster could be the source of the NW radio relic. Another subcluster is detected similar to 2 Mpc to the SE of the X-ray peak with mass M-200c =1.68(-0.20)(+0.22) x 10(14) h(70)(-1) M-circle dot. This SE subcluster is in the vicinity of the SE radio relic and may have created the SE radio relic during a past merger with the primary cluster. The fourth subcluster, M-200c = 1.87(-0.22)(+0.24) x 10(14) h(70)(-1) M-circle dot, is NW of the X-ray peak and beyond the NW radio relic.</P>

MC²: A Deeper Look at ZwCl 2341.1+0000 with Bayesian Galaxy Clustering and Weak Lensing Analyses

Benson, B.,Wittman, D. M.,Golovich, N.,Jee, M. James,van Weeren, R. J.,Dawson, W. A. American Astronomical Society 2017 The Astrophysical Journal Vol.841 No.1

<P>ZwCl 2341.1+0000, a merging galaxy cluster with disturbed X-ray morphology and widely separated (similar to 3 Mpc) double radio relics, was thought to be an extremely massive (10-30 x 10(14) M-circle dot) and complex system, with little known about its merger history. We present JVLA 2-4 GHz observations of the cluster, along with new spectroscopy from our Keck/DEIMOS survey, and apply Gaussian Mixture Modeling to the three-dimensional distribution of 227 confirmed cluster galaxies. After adopting the Bayesian Information Criterion to avoid overfitting, which we discover can bias high the total dynamical mass estimates, we find that a three-substructure model with a total dynamical mass estimate of 9.39 +/- 0.81 x 10(14) M-circle dot is favored. We also present deep Subaru imaging and perform the first weak lensing analysis on this system, obtaining a weak lensing mass estimate of 5.57 +/- 2.47 x 10(14) M-circle dot. This is a more robust estimate because it does not depend on the dynamical state of the system, which is disturbed due to the merger. Our results indicate that ZwCl 2341.1+0000 is a multiple merger system comprised of at least three substructures, with the main merger that produced the radio relics occurring near the plane of the sky, and a younger merger in the north occurring closer to the line of sight. Dynamical modeling of the main merger reproduces observed quantities (relic positions and polarizations, subcluster separation and radial velocity difference), if the merger axis angle of similar to 10(-6)(+34) degrees and the collision speed at pericenter is similar to 1900(-200)(+300) km s(-1).</P>

THE GLOBULAR CLUSTER SYSTEM OF THE COMA CD GALAXY NGC 4874 FROM<i>HUBBLE SPACE TELESCOPE</i>ACS AND WFC3/IR IMAGING

Cho, Hyejeon,Blakeslee, John P.,Chies-Santos, Ana L.,Jee, M. James,Jensen, Joseph B.,Peng, Eric W.,Lee, Young-Wook American Astronomical Society 2016 The Astrophysical journal Vol.822 No.2

<P>We present new Hubble Space Telescope (HST) optical and near-infrared (NIR) photometry of the rich globular cluster (GC) system NGC 4874, the cD galaxy in the core of the Coma cluster (Abell 1656). NGC 4874 was observed with the HST Advanced Camera for Surveys in the F475W (g(475)) and F814W (I-814) passbands and with the Wide Field Camera. 3 IR Channel in F160W (H-160). The GCs in this field exhibit a bimodal optical color distribution with more than half of the GCs falling on the red side at g(475)-I-814 > 1. Bimodality is also present, though less conspicuously, in the optical-NIR I-814-H-160 color. Consistent with past work, we find evidence for nonlinearity in the g(475)-I-814 versus I-814-H-160 color-color relation. Our results thus underscore the need for understanding the detailed form of the color-metallicity relations in interpreting observational data on GC bimodality. We also find a very strong color-magnitude trend, or 'blue tilt,' for the blue component of the optical color distribution of the NGC 4874 GC system. A similarly strong trend is present for the overall mean I-814-H-160 color as a function of magnitude; for M-814 < -10 mag, these trends imply a steep mass-metallicity scaling with Z proportional to M-GC(1.4 +/- 0.4), but the scaling is not a simple power law and becomes much weaker at lower masses. As in other similar systems, the spatial distribution of the blue GCs is more extended than that of the red GCs, partly because of blue GCs associated with surrounding cluster galaxies. In addition, the center of the GC system is displaced by 4 +/- 1 kpc toward the southwest from the luminosity center of NGC 4874, in the direction of NGC 4872. Finally, we remark on a dwarf elliptical galaxy with a noticeably asymmetrical GC distribution. Interestingly, this dwarf has a velocity of nearly -3000 km s(-1) with respect to NGC 4874; we suggest it is on its first infall into the cluster core and is undergoing stripping of its GC system by the cluster potential.</P>

MC²: Multiwavelength and Dynamical Analysis of the Merging Galaxy Cluster ZwCl 0008.8+5215: An Older and Less Massive Bullet Cluster

Golovich, Nathan,Weeren, Reinout J. van,Dawson, William A.,Jee, M. James,Wittman, David American Astronomical Society 2017 The Astrophysical journal Vol.838 No.2

<P>We present and analyze a rich data set including Subaru/SuprimeCam, HST/Advanced Camera for Surveys and Wide Field Camera 3, Keck/DEIMOS, Chandra/ACIS-I, and JVLA/C and D array for the merging cluster of galaxies ZwCl 0008.8+ 5215. With a joint Subaru+ HST weak gravitational lensing analysis, we identify two dominant subclusters and estimate the masses to be M-200 = 5.8(-1.8)(+2.8) x 10(14) M-circle dot. We estimate the projected separation between the two subclusters to be 924(-206)(+243) kpc. We perform a clustering analysis of spectroscopically confirmed cluster member galaxies and estimate the line-of-sight velocity difference between the two subclusters to be 92 +/- 164 km s(-1). We further motivate, discuss, and analyze the merger scenario through an analysis of the 42 ks of Chandra/ACIS-I and JVLA/C and D array polarization data. The X-ray surface brightness profile reveals a merging gas-core reminiscent of the Bullet Cluster. The global X-ray luminosity in the 0.5-7.0 keV band is 1.7. +/- 0.1 x 10(44) erg s(-1) and the global X-ray temperature is 4.90 +/- 0.13 keV. The radio relics are polarized up to 40%,. and along with the masses, velocities, and positions of the two subclusters, we input these quantities into a Monte Carlo dynamical analysis and estimate the merger velocity at pericenter to be 1800(-300)(+400) km s(-1). This is a lower-mass version of the Bullet Cluster and therefore may prove useful in testing alternative models of dark matter (DM). We do not find significant offsets between DM and galaxies, but the uncertainties are large with the current lensing data. Furthermore, in the east, the BCG is offset from other luminous cluster galaxies, which poses a puzzle for defining DM-galaxy offsets.</P>

COSMIC SHEAR RESULTS FROM THE DEEP LENS SURVEY. II. FULL COSMOLOGICAL PARAMETER CONSTRAINTS FROM TOMOGRAPHY

Jee, M. James,Tyson, J. Anthony,Hilbert, Stefan,Schneider, Michael D.,Schmidt, Samuel,Wittman, David American Astronomical Society 2016 The Astrophysical journal Vol.824 No.2

<P>We present a tomographic cosmic shear study from the Deep Lens Survey (DLS), which, providing a limiting magnitude r(lim) similar to 27 (5 sigma), is designed as a precursor Large Synoptic Survey Telescope (LSST) survey with an emphasis on depth. Using five tomographic redshift bins, we study their auto- and cross-correlations to constrain cosmological parameters. We use a luminosity-dependent nonlinear model to account for the astrophysical systematics originating from intrinsic alignments of galaxy shapes. We find that the cosmological leverage of the DLS is among the highest among existing > 10 deg(2) cosmic shear surveys. Combining the DLS tomography with the 9 yr results of the Wilkinson Microwave Anisotropy Probe (WMAP9) gives Omega(m) = 0.293(-0.014)(+0.012), sigma(8) = 0.833(-0.018)(+0.011), H-0 = 68.6(-1.2)(+1.4) km s(-1) Mpc(-1).4 1 1, and Omega(b) = 0.0475 +/- 0.0012 for Lambda CDM, reducing the uncertainties of the WMAP9-only constraints by similar to 50%. When we do not assume flatness for Lambda CDM, we obtain the curvature constraint Omega(k) = -0.010(-0.015)(+0.013) from the DLS+WMAP9 combination, which, however, is not well constrained when WMAP9 is used alone. The dark energy equation-of-state parameter w is tightly constrained when baryonic acoustic oscillation (BAO) data are added, yielding = - w -1.02(-0.09)(+0.10) with the DLS+WMAP9+BAO joint probe. The addition of supernova constraints further tightens the parameter to w = -1.03 +/- 0.03. Our joint constraints are fully consistent with the final Planck results and also with the predictions of a Lambda CDM universe.</P>

From Pixels to Cosmology: Weak Gravitational Lensing with Vera Rubin Observatory's Legacy Survey of Space and Time

M. James Jee 한국천문학회 2023 天文學會報 Vol.48 No.1

Probes of Dark Matter with Large Halo Colliders

M. James Jee 한국천문학회 2023 天文學會報 Vol.48 No.2

Tracing the origin of ICL with Horizon Run 5

M. James Jee 한국천문학회 2022 天文學會報 Vol.47 No.2

Weak-Lensing Detection of Intracluster Filaments in the Coma cluster Aligned with the Large-Scale Cosmic Web

Kim HyeongHan,M. James Jee,Sangjun Cha,Hyejeon Cho 한국천문학회 2023 天文學會報 Vol.48 No.2