On The Origin Of Dust In Galaxy Clusters At Low To Intermediate Redshift

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Clusters of galaxies contain an overdensity of dwarfs compared to the field. Within galaxy clusters there is also a correlation between the overdensity of dwarfs and local galaxy density, such that areas of lower galaxy density contain more dwarfs per giant. The origin of these 'extra' dwarfs is


low- and intermediate-redshift galaxy clusters is the identification of bubble-like structures in the X-ray images (McNamara et al. 2000). This phenomenon was first seen with ROSAT in the Perseus and Cygnus A clusters (Boehringer etal. 1993; Carilli,Perley, & Harris1994).These cavities are apparently associated with energy injection due

PUBLICATION LIST ApJ, 878, 68 2019, ApJ, 875, 54 Yoshiaki Ono

Low Masses and High Redshifts: The Evolution of the Mass-Metallicity Relation, Henry, A. etal. 2013, ApJ, 776, 27 Scattered Emission from z 1 Galactic Out ows, C. L. Martin etal. 2013, ApJ, 770, 41 Signatures of Cool Gas Fueling a Star-Forming Galaxy at Redshift 2.3, Bouch e, N.;

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Abstract: Globular clusters are often thought to be possible hosts of intermediate-massblackholes(IMBHs),buttheevidenceforthemisweak at best. Combining proper motions from HST and Gaia DR2 with line redshifts from VLT/MUSE, we performed mass-obit modeling with the Bayesian code MAMPOSSt-PM, which is a new extension of the public

arXiv:1007.2263v1 [astro-ph.CO] 14 Jul 2010

intermediate redshift revealed a large increase in the fraction of blue galaxies present. Spectroscopic studies have established the increased blue fraction is the re-sult of an increase in the fraction of galaxies which are actively forming stars in clusters at these redshifts (e.g. Dressler & Gunn 1982, 1983, 1992; Couch & Sharples

Disentangling the Dynamical Mechanisms for Cluster Galaxy

servations of intermediate redshift galaxies, for example, essentially only the total flux across the different IR bands are known for each cluster galaxy, with no further spatial reso-lution within a single galaxy. Therefore, given this state of the current IR observations, the new method is devised to make use

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Goulding,!A.D.,!et!al.!2014,!ApJ,!783,!40,! Tracing!the!Evolution!of!Active!Galactic! Nuclei!Host!Galaxies!over!the!Last!9!Gyr!of!Cosmic!Time !!! Graham,!M.L.,!et!al


with galaxy environment at a fixed galaxy mass. Key words: galaxies: clusters: general galaxies: evolution galaxies: formation 1. INTRODUCTION The star formation (SF) activity, like other galaxy properties, varies systematically with galaxy mass and redshift. Its trend as a function of galaxy mass has been studied in the field at


the targets low-redshift, intermediate-redshift, and high-redshift clusters of galaxies. A2255 is one of the target galaxy clusters for the low-redshift CLEVL program (Im et al. 2008; Lee et al. 2010). A2255 is observed by AKARI InfraRed Camera (IRC; Onaka et al. 2007), over eight fields (Figure 1)

A completecensusof withinthe HST FrontierFields

While the lensed, high redshift galaxies are the pri-mary interest of the HFF programme, many cluster mem-bers are also in the observations. Generally, cluster galaxies are quiescent, with little or no dust to produce FIR emis-sion. However, several Herschel studies have each detected 10s of cluster members at intermediate redshift (Rawle et al.

On the Origin of Dust in Galaxy Clusters at Low to

On the Origin of Dust in Galaxy Clusters at Low to Intermediate Redsfhift Eda Gjergo Introduction Observational Overview My work Method Results Summary Why does dust matter? I Observations of spectral energy distributions (SEDs) Figure: From Schurer A., PhD Thesis, 2009, Graph which shows the e↵ect of dust on the SED of local galaxies.

Internal kinematics of spiral galaxies in distant clusters

Galaxy clusters are important laboratories for understanding the origin of different morphological types of galaxies. The main reason for that is the relation between local galaxy density and morphological type (Dressler 1980). For nearby rich clusters, the spiral galaxy fraction decreases from 80% in the field to

Radio-selected Galaxies in Very Rich Clusters at z 0.25: I

1:4 2 1022 WHz−1) galaxy population within these extremely rich clusters for galaxies with M R −21. This is the largest sample of low luminosity 20cm radio galaxies within rich Abell clusters collected to date. The radio-selected galaxy sample represents the starburst (Star formation

The Peak Epoch of Star Formation Activity

tight photometric sequences in both low-z and intermediate-z clusters also attests to high formation redshift zf at least for the elliptical galaxy formation in dense environments (e.g., Stanford, Eisenhardt, & Dickinson 1995). Indeed, some elliptical galaxies at z ~ 1.5 are observed to contain evolved stellar


of the targets low-redshift, intermediate-redshift, and high-redshift clusters of galaxies. A2255 is one of the target galaxy clusters for the low-redshift CLEVL program (Im et al. 2008; Lee et al. 2009). A2255 is observed by the AKARI InfraRed Camera (IRC; Onaka et al. 2007) over eight fields (Figure 1), with each field

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A Multiwavelength Study of POX 52, a Dwarf Seyfert Galaxy with an Intermediate-Mass Black Hole Aaron Barth GO 10240 California Institute of Technology USA Galaxies Stars versus Gas: A Direct Comparison of Black Hole Mass Measurement Techniques Jill Bechtold AR 10318University of Arizona USA Quasar Absorption Lines

Footprints in the sand: What can globular clusters tell us

galaxy main progenitor around redshift z ≈ 2, and the metal-poor subpopulation is composed of clusters accreted from satellites, and formed at redshifts z≈3 4. In this context, the study of GCSs will help to understand the origin and evolution of ETGs in low-density environments. Distance determinations for NGC 4753 range between 20 and

Are star formation rates of galaxies bimodal?

cess. For instance, star clusters in the Milky Way have masses rang-ing from about ˘102 103 M for open clusters to ˘105 M for young massive clusters (Portegies Zwart et al.2010). Star clus-ters can be even more massive in star-bursting galaxies (Zhang & Fall1999) and at high redshift, when galaxies are generally more

Klaus Dolag USM

Virial scaling of galaxies in clusters: bright to faint is cool to hot Wu, Hahn, Evrard, Wechsler & Dolag: MNRAS 2013 Planck intermediate results. V. Pressure profiles of galaxy clusters from the Sunyaev-Zeldovich effect Planck Collaboration (incl. Dolag): A&A 2013 The Dark Halo-Spheroid Conspiracy and the Origin of Elliptical Galaxies

Recent star formation in local, morphologically disturbed

origin. A drawback of optical data is its relative insensitivity to small amounts of recent star formation (RSF). The optical spectrum re-mains largely unaffected by the minority of stellar mass that is expected to form in these systems at low and intermediate redshifts (z < 1), which makes it difficult to accurately measure early-type

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⊙) and are typically found in local densities similar to the outskirts of galaxy clusters. As much as 40% of the supercluster member galaxies in this mass range can be classified as weak-SFGs, but their proportion decreases to < 10% at larger masses (M∗ > 1010.5 M ⊙) at any galaxy density. The fraction of the intermediate-MXG among red-

The rate of supernovae at redshift 0.1-1

et al. (2012a) survey galaxy clusters, where the SN Ia rates are likely to be enhanced,to find supernovaeand have reportedcl us-ter SN rates out to redshift 0.9. Barbary et al. (2012b)also report SN Ia rates from detections in the foregroundand backgroundof the targeted galaxy clusters out to z ∼ 1.5.


Planck Intermediate Results. V. Pressure profiles of galaxy clusters from the Sunyaev-Zeldovich effect Planck Collaboration (P.A.R. Ade et al.). Jul 2012. 24 pp. e-Print: arXiv:1207.4061 [astro-ph.CO] PDF 12. Planck intermediate results. VI: The dynamical structure of PLCKG214.6+37.0, a Planck discovered triple system of galaxy clusters

of AGN Candidates I: Host-Galaxy Gas

the AGN on ≈ 50, 000-year timescales. This paper focuses on the host-galaxy properties and origin of the gas. In every galaxy, we identify evidence of ongoing or past interactions, including tidal tails, shells, and warped or chaotic dust structures; a similarly-selected sample of obscured

The star formation activity from the centers to the outskirts

formation starts already in the outskirts of clusters (at about 3Rvir), where the galaxy densities are low and the intra-cluster medium is very shallow. Galaxies with ongoing star formation have similar equivalent widths of emission lines independent of local density or clustercentric distances, suggesting that the

Dissecting Galaxies Near and Far

dedicated to galaxy groups and clusters. Jeff Kenney presented clear evidence of strong RPS in NGC 4921, the most mas-sive spiral galaxy in the Coma Cluster, with impressive Hubble Space Telescope imaging at 30 pc resolution showing a dust front of swept-up gas and dust along the leading edge of ram-pressure

Environment and Galaxy Evolution at Intermediate Redshift

Galaxy groups in this redshift range have been de ned with photometric data (de Mello Infante & Menanteau 1997) and with radio-galaxies as centers (1) but large, kinematically accurate redshift catalogs are needed to put intermediate redshift groups on the same standing as those at low redshift.

The STAGES view of red spirals and dusty red galaxies: Mass

cluster complex at redshift ∼0.17using restframe near-UV-optical SEDs, 24µm IR data and HST morphologies from the STAGES dataset. The cluster sample is based on COMBO-17 redshifts with an rms precision of σ cz ≈2000km/sec. We find that dusty red galaxies and


Optical studies of rich clusters to determine the star for-mation rates (SFRs) of their cluster members have been ongoing since the early photometric study by Butcher & Oemler (1978) over 20 years ago. Such studies have sought to recover the star formation properties of galaxies in rich clusters via optical photometry, spectroscopy, and more


Studies of the Morphological Content of Rich Clusters at Intermediate Redshift using HST 522 Warrick J. Couch Star-Forming Galaxies at z ~ 3: Bulges and Ellipticals in Their Infancy? 534 Mauro Giavalisco, Charles C. Steidel, Max Pettini, Mark E. Dickinson & Kurt L. Adelberger High-2 Objects and Cold-Dark-Matter Cosmogonies: the Case of 53W091 545

SALT Consortium PFIS Questionnaire Responses Science Goals

* intermediate-redshift cluster galaxy kinematics and stellar populations * complementary MOS of point or extended targets found in Fabry-Perot tunable filter images of quasar companions & z=1-2 galaxies * characterize star formation histories of galaxies in the redshift range 0.5 < z < 1.

High redshift radio galaxies: Beacons to biased hierarchical

clusters at low redshift,ˇ 5 10−5 h3 Mpc−3, is comparable to that of powerful AGN at z =2:5, with the interesting implication that all cluster dominant elliptical galaxies were active at z ˇ 2:5 (West 1994). The study of the low-to-intermediate redshift evolution of luminous radio galaxies is ham-strung by the paucity of such sources at


gradients in elliptical galaxies in clusters. The same conclusion has been obtained for eld elliptical gal-axies by using those at redshift 0.1¨1.0 in the Hubble Deep Field North by Tamura et al. Thus, it is also suggested that the primary origin of the color gradients in elliptical galaxies does not depend on galaxy environment.


galaxy stellar ages, star-formation timescales, stellar and gas metallicities, and dust attenuation, and infer the past evolution of galaxies at different masses and redshift, relating their star formation histories to their intrinsic (e.g., stellar mass, galaxy morphology) and environmental properties.


A low Metallicity Gas Shells surrounding the high Redshift Radio Galaxy 0943-242 109 Luc Binette, Jaron D. Kurk, Montserrat Villar-Martin & Huub J. A. Rottgering Primordial Angular Momentum Distribution in Disk Galaxies and Bulge to Disk Ratios 113 Xavier Hernandez Two pattern speeds in the barred spiral galaxy NGC 3359 117 Maite Rozas & Maria

Chapter 16

Galaxy Clusters Galaxy Clusters The Local Group Galaxy Clusters In general, all clusters need dark matter to explain galactic motions and the confinement of hot intergalactic gas within cluster Near clusters appear to have their members fairly smoothly spread out, while far away clusters (and hence younger clusters) are

University of Hawai i, Institute for Astronomy Publications

of Young Stellar Clusters, ed. T. Montmerle & P. Andre.´ Quantitative Dust Penetrated Morphological Tuning Fork at Low and High Redshift. In Galaxy Disks and Disk

Ionized gas discs in elliptical and S0 galaxies at z 1

band for the 10 intermediate-redshift cluster candidates and V, R, and I bands for the 10 high-redshift cluster candidates. In addition, near-IR J and K photometry was obtained for most clusters using SOFI at the New Technology Telescope (Aragon-Salamanca et al.,´ in preparation). We also compiled deep multislit spectroscopy with