spectral energy distribution
The Radio Spectral Energy Distribution and Star Formation Rate Calibration in Galaxies
... the spectral energy distribution (SED) of the radio continuum (RC) emission from the Key Insight in Nearby Galaxies Emitting in Radio (KINGFISHER) sample of nearby galaxies to understand the ...
24
Deriving star formation histories from photometry using energy balance spectral energy distribution modelling
... Panchromatic spectral energy distribution (SED) fitting is a critical tool for determining the physical properties of distant galaxies, such as their stellar mass and star formation ...
11
Modelling the cosmic spectral energy distribution and extragalactic background light over all time
... cosmic spectral energy distribution (CSED) and the integrated galactic light (IGL) over all cosmic ...full energy output of the Universe from the ultraviolet to the far-infrared extremely ...
19
Anatomy of the AGN in NGC 5548 I. A global model for the broadband spectral energy distribution
... the spectral energy distribution of NGC 5548 from near-infrared to hard X-rays by establishing the contribution of various emission and absorption processes taking place along our line of sight ...
18
Modelling accretion disc emission with generalized temperature profile and its effect on AGN spectral energy distribution
... broad-band spectral energy distribution (SED) of active galactic nuclei (AGNs) is investi- gated for a well-selected sample composed of 23 Seyfert 1 galaxies observed simultaneously in the ...
20
Principal Component Analysis of the Spectral Energy Distribution and Emission Line Properties of Red 2mass Active Galactic Nuclei
... The Harvard community has made this article openly available. Please share how this access benefits you. Your story matters Citation Kuraszkiewicz, Joanna, Belinda J. Wilkes, Gary Schmidt, Paul S. Smith, Roc Cutri, and ...
11
CiteSeerX — THE SPECTRAL ENERGY DISTRIBUTION OF SPIRAL GALAXIES
... Figure 6: Relations between Bolometric flux and the flux density at 25 µm (left) and 7000˚ A (right). Filled squares represent Seyfert 2’s, open squares LINER’s, filled triangles normal ellipticals, open triangles normal ...
10
The Spectral Energy Distribution of Normal, Starburst and Active Galaxies
... entire energy range, but are fainter than the other SED’s, relative to the λ7000˚ A ...entire energy range, with the exception of the ultraviolet, where SBH’s are weaker, and mid/far IR, where they are ...
29
Modelling the spectral energy distribution of super-Eddington quasars.
... to include this geometrical effects to the model. We thus still employ the thin disc geometry as is done for agnsed. One key difference is that the agnsed model assumes that the hot inner flow region does not have an ...
12
The radio spectral energy distribution of infrared-faint radio sources
... the data, even if the templates were scaled in luminosity and ex- tinction was added. The flat radio SED of the core of 3C 273 is in clear disagreement with the steep radio SEDs found for all six sources. Also the radio ...
26
The radio spectral energy distribution of infrared-faint radio sources
... Figure 6 shows the radio SED of this source – including all available data between 150 MHz and 105 GHz –, similar to the SEDs shown in Fig. 2 and in Appendix B in Fig. B.1. To de- scribe the radio emission over this wide ...
25
Reaching the peak of the quasar spectral energy distribution - I. Observations and models.
... All of the objects in our sample have either UKIRT Infrared Deep Sky Survey (UKIDSS) or 2MASS (or both) photometry in each of J, H and K bands. We first compare the flux of each pho- tometry point with the average flux ...
21
Leptonic and Hadronic Modeling of Fermi-Detected Blazars - Spectral Energy Distribution Modeling and High-Energy Polarization Predictions
... snap-shot spectral energy distributions of a representative set of Fermi-LAT detected blazars from the first LAT AGN ...kinetic energy carried by the jet should be dominated by ...
5
The HELLAS2XMM survey XIII : multi-component analysis of the spectral energy distribution of obscured AGN
... broad-band spectral energy distributions (SEDs) in order to estimate the main parameters related to the dusty torus that is assumed to be responsible for the reprocessed IR ...
14
An ALMA survey of submillimetre galaxies in the COSMOS field: Physical properties derived from energy balance spectral energy distribution modelling
... size distribution in ...stellar distribution in SMGs (see Miettinen et ...size distribution as a function of stellar mass for a subsample of our ...−R distribution of z ∼ 2 ...stellar ...
43
Galaxy And Mass Assembly : the evolution of the cosmic spectral energy distribution from z = 1 to z = 0
... Our results include appropriate errors to highlight the impact of these corrections. We show that the bolometric energy output of the Universe has declined by a factor of roughly 4 – from 5.1 ± 1.0 at z ∼ 1 to 1.3 ...
18
NuSTAR Observations and broadband spectral energy distribution modeling of the millisecond pulsar binary PSR J1023+0038
... The NuSTAR data of J1023 provide the first hard X-ray spectra extending to 79 keV for a transitional MSP/LMXB in both the MSP and LMXB states. Together with multi- wavelength observations from radio to gamma-ray, these ...
8
Nustar Observations And Broadband Spectral Energy Distribution Modeling Of The Millisecond Pulsar Binary Psr J1023+0038
... total luminosity from the pulsar wind is L pw ∼ 3 × 10 34 erg s −1 . The NuSTAR data of J1023 provide the first hard X-ray spectra extending to 79 keV for a transitional MSP/LMXB in both the MSP and LMXB states. Together ...
9
Figure 3 Spectral energy distribution emission from SgrA*. Plotted are the extinction and absorption corrected, band luminosities νlν (energy emitted
... appropriate to interpret the SgrA* infrared emission as exhibiting a range of variability amplitudes and timescales of which the observed flares are just the most extreme at present.Wir[r] ...
5
Galaxy And Mass Assembly (GAMA) : ugrizYJHK Sérsic luminosity functions and the cosmic spectral energy distribution by Hubble type.
... & Rocca-Volmerange 1999) to our data. The best fits are shown in Fig. 12 by the colour indicated in the key. The sum of these fits is shown as the black curve which agrees well with the z < 0.1 CSED showing only a slight ...
26