Surface brightness (Astronomy)
The dependence of H ii region properties on global and local surface brightness within galaxy discs
... higher surface brightness produced by the intensity of the night ...face brightness (LSB) galaxies has become its own subfield within extragalactic ...high surface brightness (HSB) ...
13
Another look at the size of the low surface brightness galaxy VCC 1661 in the Virgo Cluster
... tion that this ignores the effects of bright stars at the edge of the CCD, PSF modeling on degree-scales, and other known background variations towards Virgo such as Galactic cir- rus and Intracluster light (e.g., Mihos ...
8
A population of faint low surface brightness galaxies in the Perseus cluster core
... Does this imply that a few of the largest LSB candidates in the Perseus cluster core should be in process of tidal dis- ruption right now? – We do identify three LSB candidates in Perseus that show possible signs of ...
15
Steepening of the 820 μm continuum surface brightness profile signals dust evolution in TW Hya's disk
... dust surface density, simultaneously with the growth, fragmentation, and erosion of dust grains via grain- grain ...gas surface denisty distribution and comparison to multi-wavelength continuum ...continuum ...
8
The stability of low surface brightness disks based on multi wavelength modeling
... high surface brightness (HSB) counterparts, while their H i surface densities are lower by a factor of ∼2 (van der Hulst et ...at surface densities below the Kennicutt (1989) critical values ...
11
Surface brightness distributions of late type stars
... of surface magnetism can be derived from these re sults; for younger stars of solar mass, their rapid rotation results in a chaotic variability; for older stars (> 2 x 10® years) of solar mass, the magnetic ...
141
An Alternative Model of Rotation Curve that Explains Anomalous Orbital Velocity, Mass Discrepancy and Structure of Some Galaxies
... This now assumes that a large number of massive quakes occur in stars of each galaxy so that their orbital distances also expand due to gravitational weakening as massive tremors occur. This gives an important correction ...
7
Surface Photometry of Spiral Galaxy NGC 5005 and Elliptical Galaxy NGC 4278 Zahraa Adnan| Abdullah K. Ahmed
... of surface brightness of the compositions of the spiral galaxy NGC 5005 with the radius of the galaxy r was given uncertain values in riz-filters but the g-filter gives a good approximation to the de ...
10
Triaxial orbit-based modelling of the Milky Way Nuclear Star Cluster
... We use the triaxial orbit-based code by van den Bosch et al. (2008) to model the light distribution and line-of-sight kinematics of the Milky Way nuclear star cluster. We use the spectroscopic data cube constructed by ...
13
Photographic surface photometry of galaxies in the Virgo cluster
... Fig.2Y-— Radial luminosity distributions for N GC 4459 and M 83. I is the surface brightness. O rdi nates are log I and / in B-mag per square second of arc. R is distance from the nucleus along the major ...
766
The Herschel-ATLAS: magnifications and physical sizes of 500-μ m-selected strongly lensed galaxies
... source brightness distribution with an adaptive pixel scale scheme, extended to work in the Fourier visibility space of ...source surface brightness with an elliptical Gaussian ...
19
Spiral Arms in the Asymmetrically Illuminated Disk of MWC 758 and Constraints on Giant Planets
... disk surface. The rapid drop in surface brightness seen in the H-band PI data to the east of the spiral arms (Figure 3) further indicates that the arm is optically thick and extends sufficiently far ...
13
The bivariate space density of galaxies
... Bivariate Brightness Distribution have been ...luminosity-surface brightness relationships of 1250 galaxies from the Century Survey and Blanton et ...luminosity-surface brightness ...
236
Rybak, Matus (2017): Strong lensing with ALMA: resolving the nature of high-redshift galaxies. Dissertation, LMU München: Fakultät für Physik
... Spectral line imaging of the CO (1-0) emission from SDP.81 was carried out using the Extended Very Large Array (VLA) in the most compact D-configuration on 2010 July 18 (PI: R. Ivison; 3.3 × 2.3 arcsec beam-size at ...
127
Surface differential rotation and prominences of the Lupus post T Tauri star RX J1508.6-4423
... The brightness imaging model we chose is that of Cameron (1992) which aims at reconstructing for each point of the stellar surface a quantity f describing the local fraction of the stellar surface ...
17
The intrinsic shape and dynamical structure of the bulges of lenticular galaxies
... The latter were measured using the IRAF task ELLIPSE [13]. Starting from these initial trial parameters the different photometric models of the surface brightness were fitted iteratively to the galaxy ...
6
Science with the Australian square kilometre array pathfinder
... It is worth emphasising that at 5 resolution, incom- pleteness becomes significant as emission extended on scales larger than this is resolved (see the discussion regarding the choice of angular resolution for the NVSS ...
15
X-ray study of the double radio relic Abell 3376 with Suzaku
... Radial X-ray surface brightness profile across the eastern radio relic in the 0.3–2.0 keV band using XMM-Newton observations.. Same as Fig.[r] ...
15
Subarcsecond international LOFAR radio images of Arp 220 at 150 MHz. A kpc-scale star forming disk surrounding nuclei with shocked outflows
... nuclei. Surface brightness measurements (Table 3) are plotted as ...the surface brightness at 33 GHz positions of the two nuclei, as predicted by the three component model described in ...
18
Fading AGN candidates: AGN histories and outflow signatures
... the observed emission, making the broad assumption as noted above that the densest gas clumps are similar at various projected distances from the AGN within each system. In practice, we use the required photon rate ...
19