We assemble a database of 15 HSB and 15 LSB galaxies, for which surface brightness density and spectroscopic rotation curve data are both available and representative for various morphologies. We use this dataset to test the Navarro-Frenk-White, the Einasto, and the pseudo-isothermal sphere dark matter (DM) models. We investigate the compatibility of the pure baryonic model and baryonic plus one of the three DM models with observations on the assembled galaxy database. When a DM component improves the fit with the spectroscopic rotational curve, we rank the models according to the goodness of fit to the datasets. We constructed the spatial luminosity density of the baryonic component based on the surface brightness profile of the galaxies. We estimated the mass-to-light (M/L) ratio of the stellar component through a previously proposed color-mass-to-light ratio relation (CMLR). We assumed an axissymetric baryonic mass model with variable axis ratios together with one of the three DM models to provide the theoretical rotational velocity curves, and we compared them with the dataset. In a second attempt, we addressed the question whether the dark component could be replaced by a pure baryonic model with fitted M/L ratios. We employed the Akaike information criterion (AIC) to establish the performance of the best-fit models. For 7 galaxies, neither model fits the dataset within the 1σ confidence level. For the other 23 cases, one of the models with DM explains the rotation curve data best. According to the AIC, the PSE emerges as most favored in 14 cases, followed by the NFW (6 cases) and the Einasto (3 cases) DM models. We find that the pure baryonic model with fitted M/L ratios falls within the 1σ confidence level for 10 HSB and 2 LSB galaxies, at the price of growing the M/Ls on average by a factor of two, but the fits are inferior compared to the best-fitting DM model.
We select a volume-limited sample of galaxies derived from the SDSS-DR7 to study the environment of low surface brightness (LSB) galaxies at different scales, as well as several physical properties of the dark matter haloes where the LSB galaxies of the sample are embedded. To characterize the environment we make use of a number of publicly available value-added galaxy catalogues. We find a slight preference for LSB galaxies to be found in filaments instead of clusters, with their mean distance to the nearest filament typically larger than for high surface brightness (HSB) galaxies. The fracti…
In this paper, we use SPARC's HSBs, and LSBs galaxies to verify two issues. The first one is related to one claim of \citep{Donato} D09, namely: is the DM surface density (DMsd) a constant universal quantity, equal to $\log{(\rm Σ/M_\odot pc^{-2})}=2.15 \pm 0.2$, or does it depend on the baryon surface density of the system? The second one, is based on a MOND prediction that for HSBs the DMsd is constant, and equal to $\log{(\rm Σ/M_\odot pc^{-2})}=2.14$, while for LSBs the surface density is not constant and takes values that are smaller than for HSBs and D09 prediction \citep{Milgrom2009}. W…
The large-scale environment of low surface brightness galaxies
导致低表面亮度星系（LSB）存在的确切形成场景和演化过程尚未完全了解。由于LSB的环境以前只在小尺度（低于2 Mpc）上进行过研究，因此在更大尺度上研究LSB星系附近的星系内容可以为我们对这类星系起源的理解增加很多。我们使用SDSS DR 4的光谱主星系样本来研究LSB星系的环境星系密度，并与高表面亮度星系（HSB）附近的星系密度进行比较。环境研究，分为两个红移箱，表明低质量和更大质量的LSB都拥有比HSB更低的星系密度的环境。在2和5百万秒差距之间的尺度上，集团和细丝的尺度上，LSB和HSB之间的星系密度的差异是显着的。为了量化这一点，我们首次推出了LSB-HSB抗偏置器件。得到的LSB-HSB抗偏参数值为10%~ 15%。从这些结果中，我们得出结论，LSB形成于初始宇宙的低密度区域，直到现在一直漂移到大尺度结构的细丝和壁的外部。此外，我们的研究结果以及实际的宇宙学模拟表明，LSB是由先天和后天的混合造成的。
We present a comparative confrontation of both the Bose-Einstein Condensate (BEC) and the Navarro-Frenk-White (NFW) dark halo models with galactic rotation curves. We employ 6 High Surface Brightness (HSB), 6 Low Surface Brightness (LSB), and 7 dwarf galaxies with rotation curves falling into two classes. In the first class rotational velocities increase with radius over the observed range.The BEC and NFW models give comparable fits for HSB and LSB galaxies of this type, while for dwarf galaxies the fit is significantly better with the BEC model. In the second class the rotational velocity of …
Intermediate surface brightness (ISB) galaxies are less numerous than their counterparts at high and low surface brightness (HSB and LSB). Investigating ISB characteristics from a sample from the S4G survey, complete down to M_B=-16, we find that they have intermediate stellar, gas and baryonic masses and on average as much gas as stars. They lie on the (baryonic) Tully-Fisher relation between HSBs and LSBs, although they present a higher scatter than the latter. Their stellar to baryonic mass ratios have intermediate values unlike their condensed baryonic fractions. By comparing their environ…
The Merger-Driven Formation of Classical Low Surface Brightness Galaxies in Romulus25
Rutgers, The State University of New Jersey（新泽西州立罗格斯大学）；Johns Hopkins University（约翰斯·霍普金斯大学）；Flatiron Institute（平顶山研究所）；University College Cork（科克大学学院）；Williams College（威廉姆斯学院）；SETI Institute（搜寻地外文明研究所）；George Mason University（乔治梅森大学）；University of Washington（华盛顿大学）
We present a catalogue of an HI-selected sample of 1129 low surface brightness galaxies (LSBGs) searched from the alpha.40-SDSS DR7 survey. This sample, consisting of various types of galaxies in terms of luminosity and morphology, has extended the parameter space covered by the existing LSBG samples. Based on a subsample of 173 LSBGs which are selected from our entire LSBG sample to have the 2-horn shapes of the HI line profiles, minor-to-major axial ratios (b/a) less than 0.6 and signal-to-noise ratio (S/N) of HI detection greater than 6.5, we investigated the Tully-Fisher relation (TFr) of …
JADES: Low Surface Brightness Galaxies at 0.4 < z < 0.8 in GOODS-S
University of Arizona（亚利桑那大学）；The Pennsylvania State University（宾夕法尼亚州立大学）；University of Oxford（牛津大学）；University of California, Santa Cruz（加州大学圣克鲁兹分校）；University of Hertfordshire（赫特福德大学）；Space Telescope Science Institute（太空望远镜科学研究所）
JADES研究了0.4 < z < 0.8范围内GOODS-S地区的低表面亮度星系，分析了其恒星形成历史、尘埃消光及空间分布，发现这些星系的恒星形成率极低，可能源自z>2的共同前驱体。
SDSS-IV MaNGA: Distinct Structural Growth and Star Formation in Low and High Surface Brightness Disks
Xiamen University（厦门大学）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；Zhejiang University（浙江大学）；University of Science and Technology of China（中国科学技术大学）
We build a volume-limited sample of galaxies derived from the SDSS-DR7 to characterize several physical properties of the dark matter halos where LSB galaxies reside. Using an observational proxy for the assembly time, we found that LSB galaxies assembly half of their total halo mass later than HSB ones, reinforcing the idea of them being unevolved systems. We use 5 different methods to estimate the total halo mass, finding that the total stellar-to-halo mass ratio is up to 22% lower in LSB galaxies. Finally, in order to estimate the spin parameter, we use a bulge+disk decomposition to obtain …
We investigate the properties of the baryonic and the dark matter components in low surface brightness (LSB) disc galaxies, with central surface brightness in the B band $μ_0 \geq 23 \, mag \, arcsec^{-2}$. The sample is composed by 72 objects, whose rotation curves show an orderly trend reflecting the idea of a universal rotation curve (URC) similar to that found in the local high surface brightness (HSB) spirals in previous works. This curve relies on the mass modelling of the coadded rotation curves, involving the contribution from an exponential stellar disc and a Burkert cored dark matter…
We compare six models (including the baryonic model, two dark matter models, two modified Newtonian dynamics models and one modified gravity model) in accounting for the galaxy rotation curves. For the dark matter models, we assume NFW profile and core-modified profile for the dark halo, respectively. For the modified Newtonian dynamics models, we discuss Milgrom's MOND theory with two different interpolation functions, i.e. the standard and the simple interpolation functions. As for the modified gravity, we focus on Moffat's MSTG theory. We fit these models to the observed rotation curves of …
Massive disk galaxies with high surface brightness plus low surface brightness stellar disks, hosted by massive dark matter halo -- a TNG50 simulation study
Tata Institute of Fundamental Research（塔塔基础研究所）；Inter-University Centre for Astronomy and Astrophysics（大学间天体物理中心）
We estimate the stellar mass for a sample of low surface brightness galaxies (LSBGs) by fitting their multiband spectral energy distributions (SEDs) to the stellar population synthesis (SPS) model. The derived stellar masses (log M*/Msun) span from 7.1 to 11.1, with a mean of log M*/Msun=8.5, which is lower than that for normal galaxies. The stellar mass-to-light ratio (M/L) in each band varies little with absolute magnitude, but increases with higher M*. This trend of M/L with M* is even stronger in bluer bands. In addition, the M/L for our LSBGs slightly declines from the r band to the longe…
We argue that a natural explanation for a variety of robust galaxy scaling relations comes from the perspective of pattern formation and self-organization as a result of symmetry breaking. We propose a simple Lagrangian model that combines a conventional model for normal matter in a galaxy with a conventional model for stripe pattern formation in systems that break continuous translation invariance. We show that the energy stored in the pattern field acts as an effective dark matter. Our theory reproduces the gross features of elliptic galaxies as well as disk galaxies (HSB and LSB) including …
The GMRT archive atomic gas survey -- III. Comparative Study of Dark Matter Halos in Nearby Galaxies
Indian Institute of Science（印度科学研究所）；Indian Institute of Astrophysics（印度天体物理研究所）；Max-Planck-Institut für Radioastronomie (MPIfR)（马克斯·普朗克射电天文研究所）；Institute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences（保加利亚科学院天文学与国家天文台）；New Mexico Institute of Mining and Technology（新墨西哥矿业理工学院）；Indian Institute of Technology Indore（印度印多尔理工学院）；ASTRON – Netherlands Institute for Radio Astronomy（荷兰射电天文研究所）；National Centre for Radio Astrophysics (NCRA–TIFR)（国家射电天体物理学中心）
