Emission-line galaxies
Spectral properties of x-ray selected narrow emission line galaxies
... nearby galaxies with fluctuations in th e X -ra y background as m easured by HEAO-1 and Ginga in th e range 2-10 keV and w ith ROSAT in th e ...these galaxies them selves, or a population of unknown sources ...
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Boötes HiZELS:an optical to near infrared survey of emission line galaxies at z=0 4 4 7
... of emission-line galaxies using their Hα line at z = ...of line-emitters, their global properties such as number den- sities, the number of dual-NB emitters and X-ray detec- ...
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Evolution of Star forming Galaxies from z=0 7 to 1 2 with eBOSS Emission line Galaxies
... red galaxies (LRGs) up to z = 1.0 and the star-forming galaxies with strong nebular emission lines, ...a.k.a. emission-line galaxies (ELGs), up to z = ...
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OMEGA OSIRIS mapping of emission line galaxies in A901/2: III Galaxy properties across projected phase space in A901/2
... Khochfar & Silk 2006, 2009; Hopkins et al. 2009) and minor (e.g. Hopkins et al. 2009; Oser et al. 2012; Hilz, Naab & Ostriker 2013) mergers with other galaxies, as well as gas accretion from the halo and ...
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The Number Density Evolution of Extreme Emission Line Galaxies in 3D-HST: Results from a Novel Automated Line Search Technique for Slitless Spectroscopy
... the comoving number density toward the present epoch from our 3D-HST sample. Although the distribution for the redshift evolution β for the H α sample is wide, the value of f is well- constrained from the MCMC analysis, ...
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The ESO Nearby Abell Cluster Survey. III. Distribution and kinematics of emission-line galaxies.
... (cluster) galaxies at higher redshifts (and fainter apparent magnitudes), which therefore have an inevitable observational bias against galaxies without detectable emission lines, this bias can in ...
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OMEGA – OSIRIS Mapping of Emission line Galaxies in A901/2: II Environmental influence on integrated star formation properties and AGN activity
... sky emission, which consists of a series of sky rings around the optical centre that are a consequence of the wavelength radial ...the galaxies, a pattern that is more apparent when the images are ...mean ...
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OMEGA–OSIRIS mapping of emission line galaxies in A901/2:IV Extinction of star formation estimators with inclination
... of galaxies it causes an under- estimation of the average cosmic matter density ...of galaxies to suffer from selective incompleteness that even affects cosmological studies; finally, measurements of the ...
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X-ray Evolution and Variability of Active Galactic Nuclei
... narrow emission line galaxies (NELGs) were included in the qo = ...broad line and narrow line AGN is shown for z < ...broad line AGN when they are at higher X -ray lum ...
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Determining the halo mass scale where galaxies lose their gas
... between galaxies, the gas ejected during a merger in a dense environment is less likely to fall back onto the merged galaxy because of its interactions with the group tidal fi eld and the intragroup ...eld ...
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Abundant serendipitous emission line sources with JWST/NIRSpec
... consider emission lines apart from [O III ] and H α, our results represent a lower limit to the number of potentially observable ...rest-frame-optical emission line, [O II ] λλ3727, 3729, is commonly ...
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A dichotomy in the orientation of dust and radio jets in nearby low-power radio galaxies
... radio galaxies varies from regular elliptical shapes, evoking the idea of inclined disks, to highly irregular structures, suggest- ing unsettled ...some galaxies it is not possible to deter- mine ...
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The Distribution of Rich Clusters of Galaxies
... effects of the projected distribution along the line of sight of images of galaxies at various distances, of galaxies belonging to clusters centered outside the photograph, and of galaxi[r] ...
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Studying the [O iii]λ5007 Å Emission-line Width in a Sample of ∼ 80 Local Active Galaxies: A Surrogate For σ⋆?
... of galaxies with kinematically decoupled stellar and gaseous components with fractions as large as ∼ 30–40 per cent in elliptical and lenticular galaxies (see ...Nearby Galaxies at Apache Point ...
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Explaining the [C II]157.7 μm Deficit in Luminous Infrared Galaxies - First Results from a Herschel/PACS Study of the GOALS Sample
... the line converge with an accuracy of 1%, or when reaching 10 ...the emission lines of several sources present asymmetries and double peaks in their ...the line, it can be used as a first order ...
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The growth of typical star-forming galaxies and their supermassive black holes across cosmic time since z ~ 2
... However, our results are still fully consistent with a completely flat relation (only ∼ 1 σ away from a flat relation). This may be a sign that the BH accretion and SF of our typical star-forming galaxies evolve ...
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Cosmic explosions: the beasts and their lair
... Gamma-ray bursts are short, intense and non-thermal bursts of photons with ∼ MeV energies, which outshine the entire γ-ray sky (Klebesadel et al. 1973). GRBs were discovered serendipitously by the Vela satellites, ...
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High-precision Photometric Redshifts from Spitzer/IRAC: Extreme [3.6] - [4.5] Colors Identify Galaxies in the Redshift Range z ~ 6.6 - 6.9
... One effect that could in fl uence our estimated photometric redshifts for these objects — and possibly offer an explanation for their blue [3.6] - [4.5] colors — is the presence of high EW Ly α emission in these ...
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The Origins of [C II] Emission in Local Star-forming Galaxies
... ne-structure line is the brightest emission line observed in local star-forming ...] emission remains unclear because C + can be found in multiple phases of the interstellar ...] ...
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Reverberation mapping of optical emission lines in five active galaxies
... 5007 line fl ux is not explicitly forced to be equal from night to night, the scatter of the [ O III ] λ 5007 line light curve serves as an estimate of our calibration uncertainty ( Barth et ...5007 ...
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