scholarly journals The Frequency of Anomalously Red Galaxies in SDSS Clusters

2014 ◽  
Vol 31 ◽  
Author(s):  
O. Shearman ◽  
K. A. Pimbblet
Keyword(s):  
Surface Brightness ◽  
Dust Content ◽  
Early Type ◽  
Late Type ◽  
Cluster Membership ◽  
Cluster Galaxies ◽  
Low Surface Brightness ◽  
Magnitude Diagram ◽  
Red Galaxies ◽  
Red Sequence

AbstractWe present a systematic photometric search for spectroscopically confirmed anomalously red galaxies members of 748 low redshift clusters between 0.03 z 0.17 from the SDSS-C4 cluster catalogue (Miller et al. 2005). For each cluster we spectroscopically determine cluster membership, construct a colour-magnitude diagram and fit the red sequence using a robust bi-weight fit. We define an “anomalously red galaxy” as having a (g - r) colour of greater than 3σ redward of the fitted cluster colour-magnitude relation. We find that of 7485 galaxies at r ≤ 17.77 in (g - r), 7 galaxies are anomalously red – 0.0935 per cent of all galaxies in our sample. We show that two of the red outliers are caused by red contamination from nearby sources and are therefore not intrinsically anomalous red. However, 5 have no underlying cause to be so red and we speculate that they may have a high internal dust content. These intrinsically red galaxies are rare – comprising no more than 0.0668 per cent of all cluster galaxies. Most are morphologically early type galaxies, with a few probable late type galaxies that are viewed edge-on and one low surface brightness late type. One of our anomalously red galaxies appears to be a dust-shrouded starburst and we speculate that this may be a unique galaxy amoungst this galaxy set.

scholarly journals The haloes and environments of nearby galaxies (HERON) – I. Imaging, sample characteristics, and envelope diameters

2019 ◽  
Vol 490 (2) ◽  
pp. 1539-1569 ◽  
Author(s):  
R Michael Rich ◽  
Aleksandr Mosenkov ◽  
Henry Lee-Saunders ◽  
Andreas Koch ◽  
John Kormendy ◽  
...  
Keyword(s):  
Surface Brightness ◽  
Dwarf Galaxy ◽  
Sky Survey ◽  
Low Surface Brightness ◽  
Magnitude Diagram ◽  
The Galaxy ◽  
Nearby Galaxies ◽  
Sample Characteristics ◽  
S0 Galaxies ◽  
Red Sequence

ABSTRACT We use a dedicated 0.7-m telescope to image the haloes of 119 galaxies in the Local Volume to μr ∼ 28–30 mag arcsec−2. The sample is primarily from the Two Micron All Sky Survey Large Galaxy Atlas (Jarrett et al. 2003) and extended to include nearby dwarf galaxies and more distant giant ellipticals, and spans fully the galaxy colour–magnitude diagram including the blue cloud and red sequence. We present an initial overview, including deep images of our galaxies. Our observations reproduce previously reported low surface brightness structures, including extended plumes in M 51, and a newly discovered tidally extended dwarf galaxy in NGC 7331. Low surface brightness structures, or ‘envelopes’, exceeding 50 kpc in diameter are found mostly in galaxies with MV < −20.5, and classic interaction signatures are infrequent. Defining a halo diameter at the surface brightness 28 mag arcsec−2, we find that halo diameter is correlated with total galaxy luminosity. Extended signatures of interaction are found throughout the galaxy colour–magnitude diagram without preference for the red or blue sequences, or the green valley. Large envelopes may be found throughout the colour–magnitude diagram with some preference for the bright end of the red sequence. Spiral and S0 galaxies have broadly similar sizes, but ellipticals extend to notably greater diameters, reaching 150 kpc. We propose that the extended envelopes of disc galaxies are dominated by an extension of the disc population rather than by a classical Population II halo.

scholarly journals An expanded catalogue of low surface brightness galaxies in the Coma cluster using Subaru/Suprime-Cam

2020 ◽  
Vol 496 (3) ◽  
pp. 3182-3197
Author(s):  
Adebusola B Alabi ◽  
Aaron J Romanowsky ◽  
Duncan A Forbes ◽  
Jean P Brodie ◽  
Nobuhiro Okabe
Keyword(s):  
Surface Brightness ◽  
Structural Parameters ◽  
Imaging Data ◽  
Coma Cluster ◽  
Cluster Galaxies ◽  
Low Surface Brightness ◽  
Colour Distribution ◽  
Galaxy Population ◽  
Lsb Galaxies ◽  
Red Sequence

ABSTRACT We present a catalogue of low surface brightness (LSB) galaxies in the Coma cluster obtained from deep Subaru/Suprime-Cam V- and R-band imaging data within a region of $\mathord {\sim }4$ deg2. We increase the number of LSB galaxies presented in Yagi et al. (2016) by a factor of $\mathord {\sim }3$ and report the discovery of 29 new ultradiffuse galaxies (UDGs). We compile the largest sample of UDGs with colours and structural parameters in the Coma cluster. While most UDGs lie along the red-sequence relation of the colour–magnitude diagram, $\mathord {\sim }16$ per cent are outside (bluer or redder) the red-sequence region of Coma cluster galaxies. Our analyses show that there is no special distinction in the basic photometric parameters between UDGs and other LSB galaxies. We investigate the clustercentric colour distribution and find a remarkable transition at a projected radius of $\mathord {\sim }0.6$ Mpc. Within this cluster core region and relative to the red-sequence of galaxies, LSB galaxies are on average redder than co-spatial higher surface brightness galaxies at the 2σ level, highlighting how vulnerable LSB galaxies are to the physical processes at play in the dense central region of the cluster. The position of the transition radius agrees with expectations from recent cosmological simulation of massive galaxy clusters within which ancient infalls are predicted to dominate the LSB galaxy population.

scholarly journals An optical and H I study of late-type low surface brightness galaxies

1982 ◽  
Vol 200 (2) ◽  
pp. 325-346 ◽  
Author(s):  
A. J. Longmore ◽  
T. G. Hawarden ◽  
W. M. Goss ◽  
U. Mebold ◽  
B. L. Webster
Keyword(s):  
Surface Brightness ◽  
Late Type ◽  
Low Surface Brightness ◽  
Low Surface Brightness Galaxies

scholarly journals UV-IR color profiles of the outer regions of 2K nearby S4G galaxies

2016 ◽  
Vol 11 (S321) ◽  
pp. 257-259
Author(s):  
Alexandre Y. K. Bouquin ◽  
Armando Gil de Paz
Keyword(s):  
Surface Brightness ◽  
Large Fraction ◽  
Early Type ◽  
Late Type ◽  
Quenching Mechanism ◽  
Star Forming ◽  
Spatially Resolved ◽  
Ram Pressure ◽  
Late Type Star ◽  
Radial Evolution

AbstractWe present our new, spatially-resolved, photometry in FUV and NUV from images obtained by GALEX, and IRAC1 (3.6 μm) photometry obtained by the Spitzer Space Telescope. We analyzed the surface brightness profiles μFUV, μNUV, μ[3.6], as well as the radial evolution of the (FUV-NUV), (FUV - [3.6]), and (NUV - [3.6]) colors in the Spitzer Survey of Stellar Structures in Galaxies (S4G) galaxies (d < 40 Mpc) sample. We defined the GALEX Blue Sequence (GBS) and GALEX Red Sequence (GBR) from the (FUV - NUV) versus (NUV - [3.6]) color-color diagram, populated by late-type star forming galaxies and quiescent early-type galaxies respectively. While most disk becomes radially bluer for GBS galaxies, and stay constant for GRS galaxies, a large fraction ( > 50%) of intermediary GALEX Green Valley (GGV) galaxies’ outer disks are becoming redder. An outside-in quenching mechanism such as environmentally-related mechanisms such as starvation or ram-pressure-stripping could explain our results.

scholarly journals Evolution in cluster cores since z ~ 1

2012 ◽  
Vol 8 (S295) ◽  
pp. 172-173
Author(s):  
Claire Burke ◽  
Chris Collins ◽  
John Stott ◽  
Matt Hilton
Keyword(s):  
Surface Brightness ◽  
Large Fraction ◽  
Late Time ◽  
Cluster Galaxies ◽  
Brightest Cluster Galaxies ◽  
Size Evolution ◽  
Low Surface Brightness ◽  
Cluster Cores ◽  
Intracluster Light ◽  
Individual Galaxy

AbstractA large fraction of the stellar mass in galaxy clusters is thought to be contained in the diffuse low surface brightness intracluster light (ICL). Being bound to the gravitational potential of the cluster rather than any individual galaxy, the ICL contains much information about the evolution of its host cluster and the interactions between the galaxies within. However due its low surface brightness it is notoriously difficult to study. We present the first detection and measurement of the flux contained in the ICL at z ~ 1. We find that the fraction of the total cluster light contained in the ICL may have increased by factors of 2–4 since z ~ 1, in contrast to recent findings for the lack of mass and scale size evolution found for brightest cluster galaxies. Our results suggest that late time build-up in cluster cores may occur more through stripping than merging and we discuss the implications of our results for hierarchical simulations.

scholarly journals The Fornax Deep Survey with the VST

2019 ◽  
Vol 623 ◽  
pp. A1 ◽  
Author(s):  
E. Iodice ◽  
M. Spavone ◽  
M. Capaccioli ◽  
R. F. Peletier ◽  
G. van de Ven ◽  
...  
Keyword(s):  
Globular Clusters ◽  
Surface Brightness ◽  
Major Axis ◽  
Position Angle ◽  
Early Type ◽  
Semi Major Axis ◽  
Cluster Galaxies ◽  
The Galaxy ◽  
Deep Survey ◽  
Fornax Cluster

Context. This paper is based on the multi-band (ugri) Fornax Deep Survey (FDS) with the VLT Survey Telescope (VST). We study bright early-type galaxies (mB ≤ 15 mag) in the 9 square degrees around the core of the Fornax cluster, which covers the virial radius (Rvir  ∼ 0.7 Mpc). Aims. The main goal of the present work is to provide an analysis of the light distribution for all galaxies out to unprecedented limits (in radius and surface brightness) and to release the main products resulting from this analysis in all FDS bands. We give an initial comprehensive view of the galaxy structure and evolution as a function of the cluster environment. Methods. From the isophote fit, we derived the azimuthally averaged surface brightness profiles, the position angle, and ellipticity profiles as a function of the semi-major axis. In each band, we derived the total magnitudes, effective radii, integrated colours, and stellar mass-to-light ratios. Results. The long integration times, the arcsec-level angular resolution of OmegaCam at VST, and the large covered area of FDS allow us to map the light and colour distributions out to large galactocentric distances (up to about 10−15 Re) and surface brightness levels beyond μr = 27 mag arcsec−2 (μB ≥ 28 mag arcsec−2). Therefore, the new FDS data allow us to explore in great detail the morphology and structure of cluster galaxies out to the region of the stellar halo. The analysis presented in this paper allows us to study how the structure of galaxies and the stellar population content vary with the distance from the cluster centre. In addition to the intra-cluster features detected in previous FDS works, we found a new faint filament between FCC 143 and FCC 147, suggesting an ongoing interaction. Conclusions. The observations suggest that the Fornax cluster is not completely relaxed inside the virial radius. The bulk of the gravitational interactions between galaxies happens in the W-NW core region of the cluster, where most of the bright early-type galaxies are located and where the intra-cluster baryons (diffuse light and globular clusters) are found. We suggest that the W-NW sub-clump of galaxies results from an infalling group onto the cluster, which has modified the structure of the galaxy outskirts (making asymmetric stellar halos) and has produced the intra-cluster baryons (ICL and GCs), concentrated in this region of the cluster.

scholarly journals Galaxy Environments in DEEP2: The Birth of the Red Sequence

2006 ◽  
Vol 2 (S235) ◽  
pp. 167-169
Author(s):  
Michael C. Cooper ◽  
Jeffrey A. Newman
Keyword(s):  
Star Formation ◽  
Evolutionary Trends ◽  
Early Type ◽  
Number Density ◽  
Late Type ◽  
Active Star ◽  
The Galaxy ◽  
Blue Galaxies ◽  
Galaxy Population ◽  
Red Sequence

The galaxy population at z ≲ 1 is effectively described as a combination of two distinct types: red, early-type galaxies lacking much star formation and blue, late-type galaxies with active star formation. For the red galaxy population, recent work by Bell et al. (2004) has shown that the number density of ~L* galaxies on the red sequence has risen by a factor of ~2 from z ~ 1 to z ~ 0. A variety of complementary observations suggests that the build-up of galaxies on the red sequence results from 2 distinct evolutionary trends: (1) the quenching of star formation in blue galaxies and their subsequent migration onto the red sequence and (2) the dissipationless or (“dry”) merging of red-sequence galaxies.

scholarly journals Optical Counterparts to Galaxies in the Cen A Group Discovered by HIPASS

1999 ◽  
Vol 16 (1) ◽  
pp. 60-65 ◽  
Author(s):  
Patricia M. Knezek
Keyword(s):  
Surface Brightness ◽  
Survey Area ◽  
Late Type ◽  
New Members ◽  
Low Surface Brightness ◽  
Survey Technique ◽  
Group Members ◽  
The Subject ◽  
Centaurus A

AbstractWe have completed a 21-cm survey of a 600 square degree region of the Centaurus A group of galaxies at a redshift of ∼500 km s−1 as part of a larger survey of the entire southern sky. This group of galaxies was recently the subject of a separate and thorough optical survey (Côté et al. 1997), and thus presented an ideal comparison for us to test the survey performance. We have identified 10 new group members to add to the 21 already known in our survey area. Six of the new members are previously uncatalogued galaxies, while four were catalogued but assumed not to be group members. Including the seven known members outside of our survey area, this brings the total known number of Cen A members to 38. All of the new HI detections have optical counterparts, most being intrinsically very faint (MB > –13·0), late-type low surface brightness dwarfs. Most of the new members have HI masses only a few times our survey limit of 107M☉ at an assumed distance for the group of 3·5 Mpc, and are extremely gas-rich, with a median MHI/LB > 1. Our limiting HI sensitivity was actually slightly worse than the HI follow-up observations of the Côté et al. optical survey, yet we have already increased the known number of group members by 50% using an HIsurvey technique. While we have increased the known number of members by ∼50%, these new members contribute <4% to its light.

scholarly journals Galaxy properties from voids to clusters in the SDSS-DR4

2006 ◽  
Vol 2 (S235) ◽  
pp. 243-243
Author(s):  
G. Sorrentino ◽  
A. Rifatto ◽  
V. Antonuccio-Delogu
Keyword(s):  
Early Type ◽  
Late Type ◽  
Cluster Galaxies ◽  
Galaxy Populations ◽  
Galaxy Population ◽  
Environmental Dependence

AbstractWe investigate the environmental dependence of galaxy populations properties in the SDSS-DR4. Our aim is to search for systematic variations in the properties of galaxies with the local galaxy density in order to find hints that can be related to the presence of a void galaxy population. We find that galaxies in underdense regions (voids) are fainte and bluer than cluster galaxies. Moreover, the transition from underdense to overdense regions is smooth, as well as the percentage of late-type galaxies decreases while the percentage of early-type galaxies increases smoothly from underdense to dense environments.

scholarly journals Detections of CO in Late-Type, Low Surface Brightness Spiral Galaxies

2005 ◽  
Vol 129 (4) ◽  
pp. 1849-1862 ◽  
Author(s):  
Lynn D. Matthews ◽  
Yu Gao ◽  
Juan M. Uson ◽  
Françoise Combes
Keyword(s):  
Surface Brightness ◽  
Spiral Galaxies ◽  
Late Type ◽  
Low Surface Brightness
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