Evolution of bulgeless low surface brightness galaxies

2015 ◽  
Vol 11 (S319) ◽  
pp. 138-138
Author(s):  
X. Shao ◽  
F. Hammer ◽  
Y. B. Yang ◽  
Y. C. Liang
Keyword(s):  
Surface Brightness ◽  
Large Scale ◽  
Stellar Population ◽  
Young Stars ◽  
Sloan Digital Sky Survey ◽  
Limited Sample ◽  
Sky Survey ◽  
Low Surface Brightness ◽  
Low Surface Brightness Galaxies ◽  
Lsb Galaxies

AbstractBased on the Sloan Digital Sky Survey DR 7, we investigate the environment, morphology, and stellar population of bulgeless low surface-brightness (LSB) galaxies in a volume-limited sample with redshift ranging from 0.024 to 0.04 and Mr ≤ −18.8. We find that, for bulgeless galaxies, the surface brightness does not depend on the environment. Irregular LSB galaxies have more young stars and are more metal-poor than regular LSB galaxies. These results suggest that the evolution of LSB galaxies may be driven by their dynamics, including mergers rather than by their large-scale environment.

scholarly journals Linking Clustering Properties and the Evolution of Low Surface Brightness Galaxies

2007 ◽  
Vol 3 (S244) ◽  
pp. 274-278
Author(s):  
Dominik J. Bomans ◽  
S. Dominik Rosenbaum
Keyword(s):  
Galaxy Evolution ◽  
Surface Brightness ◽  
Large Scale ◽  
High Surface ◽  
Sloan Digital Sky Survey ◽  
Dark Matter Halo ◽  
Sky Survey ◽  
Low Surface Brightness ◽  
Low Surface Brightness Galaxies ◽  
Lsb Galaxies

AbstractThe reasons for the presence of two branches of galaxy evolution, one producing high surface brightness disks and one creating low surface brightness disks, is still unknown. Possible are the imprint of the properties of the dark matter halo, as well as evolutionary effects. In this paper we present an analysis of the clustering properties of LSB and HSB galaxies using the Sloan Digital Sky Survey. We show that LSB galaxies reside in regions of lower galaxy density than HSB galaxies on all scales between 0.8 and 8 Mpc, from scales of galaxy pairs to filaments of the Large Scale Structure. This implies a probable scenario of LSB galaxies preferentially forming as a result of local peaks in the large-scale valleys of the primordial density distribution.

scholarly journals Stellar Population Analysis on a Large Sample of Low Surface Brightness Galaxies

2012 ◽  
Vol 8 (S292) ◽  
pp. 154-154 ◽  
Author(s):  
Xiaoyan Chen ◽  
Ali Luo ◽  
Yanchun Liang
Keyword(s):  
Surface Brightness ◽  
Stellar Population ◽  
Population Analysis ◽  
Sloan Digital Sky Survey ◽  
Large Sample ◽  
Central Surface ◽  
Sky Survey ◽  
Low Surface Brightness ◽  
Galaxy Sample ◽  
Low Surface Brightness Galaxies

AbstractWe study the stellar populations of a large sample of nearly face-on disk Low Surface Brightness Galaxies (LSBGs), with B-band central surface brightness μ0(B) > 22 mag arcsec−2, selected from the Sloan Digital Sky Survey Data Release 4 (SDSS-DR4) main galaxy sample (similar to Zhong et al. 2008; Liang et al. 2010).

scholarly journals Low surface brightness galaxies in z > 1 galaxy clusters: HST approaching the progenitors of local ultra diffuse galaxies

2021 ◽  
Vol 646 ◽  
pp. L12
Author(s):  
Aisha Bachmann ◽  
Remco F. J. van der Burg ◽  
Jérémy Fensch ◽  
Gabriel Brammer ◽  
Adam Muzzin
Keyword(s):  
Surface Brightness ◽  
Stellar Population ◽  
Formation Mechanisms ◽  
Population Modelling ◽  
Local Scaling ◽  
Size Evolution ◽  
Low Surface Brightness ◽  
Hydrodynamical Simulations ◽  
Low Surface Brightness Galaxies ◽  
Lsb Galaxies

Ultra diffuse galaxies (UDGs) are a type of large low surface brightness (LSB) galaxies with particularly large effective radii (reff >  1.5 kpc) that are now routinely studied in the Local (z <  0.1) Universe. While they are found to be abundant in clusters, groups, and in the field, their formation mechanisms remain elusive and comprise an active topic of debate. New insights may be found by studying their counterparts at higher redshifts (z >  1.0), even though cosmological surface brightness dimming makes them particularly difficult to detect and study in this channel. In this work, we use the deepest Hubble Space Telescope (HST) imaging stacks of z >  1 clusters, namely, SPT-CL J2106−5844 and MOO J1014+0038. These two clusters, at z = 1.13 and z = 1.23, respectively, were monitored as part of the HST See-Change programme. In making a comparison with the Hubble Extreme Deep Field as the reference field, we find statistical over-densities of large LSB galaxies in both clusters. Based on stellar-population modelling and assuming no size evolution, we find that the faintest sources we can detect are about as bright as expected for the progenitors of the brightest local UDGs. We find that the LSBs we detect in SPT-CL J2106−5844 and MOO J1014−5844 already have old stellar populations that place them on the red sequence. In correcting for incompleteness and based on an extrapolation of local scaling relations, we estimate that distant UDGs are relatively under-abundant, as compared to local UDGs, by a factor ∼3. A plausible explanation for the implied increase over time would be the significant growth of these galaxies over the last ∼8 Gyr, as also suggested by hydrodynamical simulations.

scholarly journals Low Surface Brightness Galaxies in the Sloan Digital Sky Survey. I. Search Method and Test Sample

2004 ◽  
Vol 127 (2) ◽  
pp. 704-727 ◽  
Author(s):  
Alexei Y. Kniazev ◽  
Eva K. Grebel ◽  
Simon A. Pustilnik ◽  
Alexander G. Pramskij ◽  
Tamara F. Kniazeva ◽  
...  
Keyword(s):  
Surface Brightness ◽  
Test Sample ◽  
Search Method ◽  
Sloan Digital Sky Survey ◽  
Sky Survey ◽  
Low Surface Brightness ◽  
Low Surface Brightness Galaxies

scholarly journals Low Surface Brightness Galaxies Around the Hubble Deep Field South

2007 ◽  
Vol 3 (S244) ◽  
pp. 354-355 ◽  
Author(s):  
L. Haberzettl ◽  
D. J. Bomans ◽  
R.-J. Dettmar
Keyword(s):  
Star Formation ◽  
Surface Brightness ◽  
Stellar Population ◽  
Stellar Populations ◽  
Low Surface Brightness ◽  
Galaxy Redshift ◽  
Low Surface Brightness Galaxies ◽  
Hubble Deep Field ◽  
Lsb Galaxies ◽  
Selection Of

AbstractWe present results from a study of the SFH of a sample of LSB galaxies around the HDF-S. For the selection of the LSB galaxy candidates we used color–color diagrams, from which we selected the candidates based on their different location in comparison to the HSB galaxy redshift tracks. We compared measured spectra to synthetic SEDs from synthesis evolution models. We were able to fit SEDs in the range of 2 to 5 Gyr to the spectra of the LSB galaxies, while applying the same method to a sample of HSB galaxies resulted in an averaged stellar population of about 10 to 14 Gyr. Therefore, LSB galaxies tend to show much younger averaged stellar populations. This implies that the major star formation event of LSB galaxies took place at a redshift of z ~ 0.2 to 0.4 while for HSB galaxies this tends to be at z ~ 2 to 4.

scholarly journals Edge-on Low Surface Brightness Galaxies in the SDSS and the Red Halo Phenomenon

2006 ◽  
Vol 2 (S235) ◽  
pp. 82-82
Author(s):  
Brady Caldwell ◽  
Nils Bergvall
Keyword(s):  
Surface Brightness ◽  
Stellar Population ◽  
High Surface ◽  
Disk Galaxies ◽  
High Surface Brightness ◽  
Polar Direction ◽  
Low Surface Brightness ◽  
Compact Galaxies ◽  
Low Surface Brightness Galaxies ◽  
Lsb Galaxies

AbstractExtremely red halos have been detected around high surface brightness (HSB) disk galaxies and blue compact galaxies. We analyse the halo emission of a sample of 970 stacked edge-on low surface brightness (LSB) galaxies in the SDSS (DR4) down to μg ~ 30 mag arcsec−2. These are divided by g − r colour limits into a “blue” Sample A (336 galaxies), “yellow” Sample B (318 galaxies) and “red” Sample C (316 galaxies). The gri colours indicate a prominent red excess in the polar direction, strongly deviating from any normal stellar population.

scholarly journals Surveys of Low Surface Brightness Galaxies by 4415 Films

1994 ◽  
Vol 161 ◽  
pp. 541-544
Author(s):  
S. Phillipps ◽  
Q.A. Parker
Keyword(s):  
Surface Brightness ◽  
Signal To Noise ◽  
The Past ◽  
Cluster Area ◽  
Sky Survey ◽  
Low Surface Brightness ◽  
Low Surface Brightness Galaxies

During the past few years there have been a number of surveys for low surface brightness galaxies (LSBGs). Searches using both photographic and CCD data have shown that LSBGs are actually very numerous (Impey, Bothun &amp; Malin 1987; Irwin et al. 1990). However, they are seriously biased against in any random sky survey, and even in a cluster area there are inherent size and signal-to-noise problems. The number of objects we can detect are therefore limited in two ways.

scholarly journals Low Surface Brightness Galaxies in Deep Surveys

1999 ◽  
Vol 171 ◽  
pp. 76-83
Author(s):  
Henry C. Ferguson
Keyword(s):  
Surface Brightness ◽  
Dwarf Galaxies ◽  
Recent Literature ◽  
Solid Angle ◽  
Large Space ◽  
Space Density ◽  
Faint Galaxy ◽  
Low Surface Brightness ◽  
Low Surface Brightness Galaxies ◽  
Lsb Galaxies

AbstractWe examine the constraints that can be placed on the space density of low-surface-brightness galaxies from deep HST images. Such images, while covering only a small solid angle, provide enough depth and spatial resolution to detect LSB galaxies at moderate redshift and distinguish them from galaxies of higher surface brightness.We consider five simple models of the non-evolving or slowly-evolving population of LSB galaxies, motivated by various discussions in the recent literature. The basic results are (1) models with a large space-density of giant LSB galaxies at moderate redshift do not look like the real world and, (2) models with a large space-density of dwarf LSB galaxies are consistent with HST data (that is, they do not produce more faint LSB galaxies per unit solid angle than are detected at magnitudes I ≳ 23), but these LSB dwarf galaxies do not contribute much to faint galaxy counts unless they formed their stars in a rapid burst.

scholarly journals Hα and FUV luminosities from a stochastically formed stellar population

2011 ◽  
Vol 7 (S284) ◽  
pp. 53-55
Author(s):  
Nidia Lugo Lopez L. ◽  
Gladis Magris C. ◽  
Antonio Parravano
Keyword(s):  
Power Law ◽  
Surface Brightness ◽  
Stellar Population ◽  
Mass Function ◽  
Initial Mass Function ◽  
Initial Mass ◽  
Low Surface Brightness ◽  
Low Surface Brightness Galaxies

AbstractIt has been observed that the ratio of Hα to FUV luminosity (LHα/LFUV) is lower in low surface brightness galaxies. This behaviour has been attributed to systematic variations of the upper mass end and/or the slope of the Initial Mass Function (IMF) Meurer et al. (2009) and Lee et al. (2009)). However these hypotheses do not explain the observed scatter in luminosity ratio (LHα/LFUV). We present a model for the total LHα and LFUV luminosity arising from a randomly populated IMF following the Salpeter power law and the clustering law of Oey & Clarke (2007).

Sign in / Sign up

Export Citation Format

Share Document