scholarly journals The I band Tully-Fisher relation for cluster galaxies: data presentation.

1997 ◽  
Vol 113 ◽  
pp. 22 ◽  
Author(s):  
R. Giovanelli ◽  
M. P. Haynes ◽  
T. Herter ◽  
N. P. Vogt ◽  
G. Wegner ◽  
...  
Keyword(s):  
Data Presentation ◽  
Cluster Galaxies ◽  
Fisher Relation

scholarly journals The I Band Tully-Fisher Relation for Cluster Galaxies: a Template Relation, its Scatter and Bias Corrections.

1997 ◽  
Vol 113 ◽  
pp. 53 ◽  
Author(s):  
Riccardo Giovanelli ◽  
Martha P. Haynes ◽  
Terry Herter ◽  
Nicole P. Vogt ◽  
Luiz N. da Costa ◽  
...  
Keyword(s):  
Cluster Galaxies ◽  
Fisher Relation ◽  
Bias Corrections

scholarly journals Kinematics of disk galaxies in (proto-)clusters at z = 1.5

2020 ◽  
Vol 633 ◽  
pp. A131 ◽  
Author(s):  
A. Böhm ◽  
B. L. Ziegler ◽  
J. M. Pérez-Martínez ◽  
T. Kodama ◽  
M. Hayashi ◽  
...  
Keyword(s):  
Star Formation ◽  
Galaxy Evolution ◽  
Rotation Velocity ◽  
Velocity Fields ◽  
Selection Strategy ◽  
Cluster Galaxy ◽  
Cluster Galaxies ◽  
Strategic Program ◽  
Fisher Relation ◽  
The Impact

Aims. While many aspects of the impact of dense environments on late-type galaxies at redshifts below unity have been scrutinized in the past few decades, observational studies of the interplay between environment and disk galaxy evolution at z >  1 are still scarce. We observed star-forming galaxies at z ≈ 1.5 selected from the HyperSuprimeCam Subaru Strategic Program. The galaxies are part of two significant overdensities of [O II] emitters identified via narrowband imaging and photometric redshifts from grizy photometry. Methods. We used the K-band Multi-Object Spectrograph (KMOS) to carry out Hα integral field spectroscopy of 46 galaxies in total. Ionized gas maps, star formation rates, and velocity fields were derived from the Hα emission line. We quantified morphological and kinematical asymmetries in order to look for potential gravitational (e.g., galaxy-galaxy) or hydrodynamical (e.g., ram-pressure) interactions. Results. Hα emission was detected in 36 of our targets. Of these galaxies, 34 are members of two (proto-)clusters at z = 1.47, confirming our selection strategy to be highly efficient. By fitting model velocity fields to the observed ones, we determined the intrinsic maximum rotation velocity Vmax of 14 galaxies. Utilizing the luminosity–velocity (Tully–Fisher) relation, we find that these galaxies are more luminous than their local counterparts of similar mass by up to ∼4 mag in the rest-frame B-band. In contrast to field galaxies at z <  1, the offsets of the z ≈ 1.5 (proto-)cluster galaxies from the local Tully–Fisher relation are not correlated with their star formation rates but with the ratio between Vmax and gas velocity dispersion σg. This probably reflects that fewer disks have settled to purely rotational kinematics and high Vmax/σg ratios, as is observed in the field at similar redshifts. Tests with degraded low-redshift cluster galaxy data show that we cannot identify purely hydrodynamical interactions with the imaging currently at hand. Due to relatively low galaxy velocity dispersions (σv <  400 km s−1) of the (proto-)clusters, gravitational interactions are likely more efficient, resulting in higher kinematical asymmetries than in present-days clusters.

scholarly journals The Tully-Fisher relation: evolution with redshift and environment

2006 ◽  
Vol 2 (S235) ◽  
pp. 8-11 ◽  
Author(s):  
Alfonso Aragón-Salamanca
Keyword(s):  
Spiral Galaxies ◽  
Rotation Velocity ◽  
Disk Galaxies ◽  
Cluster Galaxies ◽  
Fundamental Properties ◽  
Look Back ◽  
Formation And Evolution ◽  
Fisher Relation

AbstractThe Tully-Fisher Relation (TFR) links two fundamental properties of disk galaxies: their luminosity and their rotation velocity (mass). The pioneering work of Vogt et al. in the 1990's showed that it is possible to study the TFR for spiral galaxies at considerable look-back-times, and use it as a powerful probe of their evolution. In recent years, several groups have studied the TFR for galaxies in different environments reaching redshifts beyond one. In this brief review I summarise the main results of some of these studies and their consequences for our understanding of the formation and evolution of disk galaxies. Particular emphasis is placed on the possible environment-driven differences in the behaviour of the TFR for field and cluster galaxies.

scholarly journals Integral field observations of distant cluster galaxies

2006 ◽  
Vol 2 (S237) ◽  
pp. 489-489
Author(s):  
D. Vergani ◽  
C. Balkowski ◽  
H. Flores ◽  
V. Cayatte ◽  
F. Hammer ◽  
...  
Keyword(s):  
Structural Parameters ◽  
High Angular Resolution ◽  
Cluster Galaxies ◽  
Spatially Resolved ◽  
Optical Images ◽  
Local Measurements ◽  
Fisher Relation ◽  
Field Unit ◽  
Stellar Masses ◽  
Integral Field

AbstractWe have used the FLAMES multi-integral field unit system of the European Southern Observatory (VLT) centered on the cluster MS0451.6-0305 at z = 0.5386 to obtain the spatially resolved kinematics of the cluster members. The spectral data are supported by HST/ACS images that provide immediate morphological information of the cluster galaxies. The relevant structural parameters such as inclination, size, and orientation derived from optical high angular resolution images are compared with those derived from the kinematics. Our final goals are: 1. to derive the Tully-Fisher relation for cluster galaxies with regular kinematics. 2. to obtain the dynamical masses from resolved kinematics and stellar masses from optical images to be compared with local measurements.

scholarly journals Galaxy kinematics across different environments in the RXJ1347−1145 cluster complex

2020 ◽  
Vol 637 ◽  
pp. A30
Author(s):  
J. M. Pérez-Martínez ◽  
B. Ziegler ◽  
A. Böhm ◽  
M. Verdugo
Keyword(s):  
Star Formation ◽  
Galaxy Evolution ◽  
Formation Rate ◽  
Stellar Mass ◽  
Cluster Complex ◽  
Mass Relation ◽  
Cluster Membership ◽  
Cluster Galaxies ◽  
Fisher Relation

Aims. In order to understand the role of the different processes that drive galaxy evolution in clusters, we need comprehensive studies that simultaneously examine several of the most important physical properties of galaxies. In this work we study the interplay between the kinematic state and star formation activity of galaxies in the RXJ1347−1145 cluster complex at z ∼ 0.45. Methods. We used VLT/VIMOS to obtain slit spectra for 95 galaxies across the 40′ × 40′ area where the RXJ1347−1145 cluster complex resides. We determined the cluster membership of our targets by identifying one or more of the available emission lines within the wavelength range. Our spectroscopy is complemented with archival SUBARU/Suprime-Cam deep photometric observations in five optical bands (B, V, Rc, Ic, z′). We examined the kinematic properties of our sample attending to the degree of distortion of the extracted rotation curves. Regular rotating galaxies were included in our Tully–Fisher analysis while the distorted ones were used to study the role of cluster-specific interactions with respect to star formation and AGN activity. Results. Our analysis confirmed the cluster membership for approximately half of our targets. We report a higher fraction of galaxies with irregular gas kinematics in the cluster environment than in the field. Cluster galaxies with regular rotation display a moderate brightening in the B-band Tully–Fisher relation compatible with the gradual evolution of the stellar populations with lookback time, and no significant evolution in the stellar-mass Tully–Fisher relation, in line with previous studies at similar redshift. Average specific star formation rate values are slightly lower in our cluster sample (−0.15 dex) with respect to the main sequence of star-forming galaxies, confirming the role of the environment in the early quenching of star formation in clusters. Finally, we carried out an exploratory observational study on the stellar-to-halo mass relation finding that cluster galaxies tend to have slightly lower stellar mass values for a fixed halo mass compared to their field counterparts.

scholarly journals The Tully-Fisher relation of intermediate redshift field and cluster galaxies from Subaru spectroscopy

2006 ◽  
Vol 366 (1) ◽  
pp. 144-162 ◽  
Author(s):  
O. Nakamura ◽  
A. Aragon-Salamanca ◽  
B. Milvang-Jensen ◽  
N. Arimoto ◽  
C. Ikuta ◽  
...  
Keyword(s):  
Cluster Galaxies ◽  
Fisher Relation ◽  
Intermediate Redshift

scholarly journals Linking star formation and galaxy kinematics in the massive cluster Abell 2163

2014 ◽  
Vol 10 (S309) ◽  
pp. 330-330
Author(s):  
Veronica Menacho ◽  
Miguel Verdugo
Keyword(s):  
Star Formation ◽  
Galaxy Evolution ◽  
Structural Parameters ◽  
High Resolution Spectroscopy ◽  
Cluster Galaxies ◽  
The Galaxy ◽  
Galaxy Kinematics ◽  
Massive Halos ◽  
Fisher Relation ◽  
Stellar Masses

AbstractThe origin of the morphology-density relation is still an open question in galaxy evolution. It is most likely driven by the combination of the efficient star formation in the highest peaks of the mass distribution at high-z and the transformation by environmental processes at later times as galaxies fall into more massive halos. To gain additional insights about these processes we study the kinematics, star formation and structural properties of galaxies in Abell 2163 a very massive (~4×1015 M⊙, Holz & Perlmutter 2012) merging cluster at z = 0.2.We use high resolution spectroscopy with VLT/VIMOS to derive rotation curves and dynamical masses for galaxies that show regular kinematics. Galaxies that show irregular rotation are also analysed to study the origin of their distortion. This information is combined with stellar masses and structural parameters obtained from high quality CFHT imaging. From narrow band photometry (2.2m/WFI), centered on the redshifted Hα line, we obtain star formation rates.Although our sample is still small, field and cluster galaxies lie in a similar Tully-Fisher relation as local galaxies. Controlling by additional parameters like SFRs or bulge-to-disk ratio do not affect this result. We find however that ~50% of the cluster galaxies display irregular kinematics in contrast to what is found in the field at similar redshifts (~30%, Böhm et al.2004) and in agreement with other studies in clusters (e.g. Bösch et al.2013, Kutdemir et al.2010) which points out to additional processes operating in clusters that distort the galaxy kinematics.

scholarly journals The Tully—Fisher relation of distant cluster galaxies

2005 ◽  
Vol 361 (1) ◽  
pp. 109-127 ◽  
Author(s):  
S. P. Bamford ◽  
B. Milvang-Jensen ◽  
A. Aragón-Salamanca ◽  
L. Simard
Keyword(s):  
Distant Cluster ◽  
Cluster Galaxies ◽  
Fisher Relation

INDONESIA LANGUAGE INTERFERENCE FORM IN BASIC PPL LEARNING THAILAND UNHASY COLLEGE SYUDENTS

2020 ◽  
Vol 8 (2) ◽  
pp. 38
Author(s):  
Siti Mariana Ulfa
Keyword(s):  
Qualitative Research ◽  
Data Analysis ◽  
Data Collection ◽  
Teaching Practice ◽  
Data Presentation ◽  
Analysis Techniques ◽  
Thai Students ◽  
The Impact ◽  
Collection Methods ◽  
Recording Techniques

AbstractHumans on earth need social interaction with others. Humans can use more than one language in communication. Thus, the impact that arises when the use of one or more languages is the contact between languages. One obvious form of contact between languages is interference. Interference can occur at all levels of life. As in this study, namely Indonesian Language Interference in Learning PPL Basic Thailand Unhasy Students. This study contains the form of interference that occurs in Thai students who are conducting teaching practices in the classroom. This type of research is descriptive qualitative research that seeks to describe any interference that occurs in the speech of Thai students when teaching practice. Data collection methods in this study are (1) observation techniques, (2) audio-visual recording techniques using CCTV and (3) recording techniques, by recording all data that has been obtained. Whereas the data wetness uses, (1) data triangulation, (2) improvement in perseverance and (3) peer review through discussion. Data analysis techniques in this study are (1) data collection, (2) data reduction, (3) data presentation and (4) conclusions. It can be seen that the interference that occurs includes (1) interference in phonological systems, (2) interference in morphological systems and (3) interference in syntactic systems. 

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