The optical luminosity function of a 60-micron flux-limited sample of IRAS galaxies
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A determination is made of the optical luminosity function (OPLF) of an infrared flux-limited sample of IRAS galaxies. The sample includes 92 objects; among these are an infrared-loud quasar and two previously known Seyferts. The OPLF of the IRAS galaxies in the sample shows that in the magnitude range between -22 and 18, IRAS galaxies represent about 15 percent of field galaxies. At low luminosities, Mj greater than -19 mag, there may be a deficiency of IRAS galaxies relative to the field galaxies. The far-IR luminosity function of the sample is also derived; it agrees well with other determinations.Keywords:
Sample (material)
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Views Icon Views Article contents Figures & tables Video Audio Supplementary Data Peer Review Share Icon Share Twitter Facebook Reddit LinkedIn Tools Icon Tools Reprints and Permissions Cite Icon Cite Search Site Citation H. Zitouni, F. Daigne, R. Mochkovitch; The GRB luminosity function: prediction of the internal shock model and comparison to observations. AIP Conf. Proc. 22 May 2008; 1000 (1): 64–67. https://doi.org/10.1063/1.2943551 Download citation file: Ris (Zotero) Reference Manager EasyBib Bookends Mendeley Papers EndNote RefWorks BibTex toolbar search Search Dropdown Menu toolbar search search input Search input auto suggest filter your search All ContentAIP Publishing PortfolioAIP Conference Proceedings Search Advanced Search |Citation Search
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We construct and examine the pulsar luminosity function using the new list which includes data for 1328 radio pulsars. In this work, the luminosity function for 1400 MHz is constructed for the rst time. We also present an improved luminosity function for 400 MHz. The luminosity functions at 400 and 1400 MHz are compared. Also, the luminosity functions excluding the binary millisecond pulsars and the pulsars with low magnetic elds are constructed. It is found that the new luminosity function is considerably atter in the low luminosity part for 400 MHz. 1400 HMz luminosity values of radio pulsars together with upper limits of 1400 MHz luminosity for anomalous X-ray pulsars and dim radio quiet neutron stars are presented as a function of both characteristic age and magnetic eld. The implications of the pulsar luminosity function for these new kinds of neutron star are discussed.
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Previous studies of the Na I D interstellar absorption line doublet have shown that galactic winds occur in most galaxies with high infrared luminosities. However, in infrared-bright composite systems where a starburst coexists with an active galactic nucleus (AGN), it is unclear whether the starburst, the AGN, or both are driving the outflows. The present paper describes the results from a search for outflows in 35 infrared-faint Seyferts with 10{sup 9.9}< L{sub IR}/L{sub sun} < 10{sup 11}, or, equivalently, star formation rates (SFRs) of approx0.4-9 M{sub sun} yr{sup -1}, to attempt to isolate the source of the outflow. We find that the outflow detection rates for the infrared-faint Seyfert 1s (6%) and Seyfert 2s (18%) are lower than previously reported for infrared-luminous Seyfert 1s (50%) and Seyfert 2s (45%). The outflow kinematics of infrared-faint and infrared-bright Seyfert 2 galaxies resemble those of starburst galaxies, while the outflow velocities in Seyfert 1 galaxies are significantly larger. Taken together, these results suggest that the AGN does not play a significant role in driving the outflows in most infrared-faint and infrared-bright systems, except the high-velocity outflows seen in Seyfert 1 galaxies. Another striking result of this study is the high rate of detectionmore » of inflows in infrared-faint galaxies (39% of Seyfert 1s, 35% of Seyfert 2s), significantly larger than in infrared-luminous Seyferts (15%). This inflow may be contributing to the feeding of the AGN in these galaxies, and potentially provides more than enough material to power the observed nuclear activity over typical AGN lifetimes.« less
Outflow
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The properties of very low luminosity active galactic nuclei are not well studied, and, in particular, their possible contribution to the diffuse X-ray background is not known. In the present investigation, an X-ray luminosity function for the range from 10 to the 39th to 10 to the 42.5th ergs/s is constructed. The obtained X-ray luminosity function is integrated to estimate the contribution of these very low luminosity active galaxies to the diffuse X-ray background. The construction of the X-ray luminosity function is based on data obtained by Keel (1983) and some simple assumptions about optical and X-ray properties.
Mass-to-light ratio
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Aims. To study the cosmological evolution of active galactic nuclei (AGN) is one of the main goals of X-ray surveys. To accurately determine the intrinsic (before absorption) X-ray luminosity function, it is essential to constrain the evolutionary properties of AGN and therefore the history of the formation of supermassive black holes with cosmic time. Methods. In this paper we investigate the X-ray luminosity function of absorbed (log NH > 22) and unabsorbed AGN in three energy bands (soft: 0.5−2 keV, hard: 2−10 keV and ultrahard: 4.5−7.5 keV). For the hard and ultrahard sources we have also studied the NH function and the dependence of the fraction of absorbed AGN on luminosity and redshift. This investigation is carried out using the XMS survey along with other highly complete flux-limited deeper and shallower surveys in all three bands for a total of 1009, 435, and 119 sources in the soft, hard and ultrahard bands, respectively. We modelled the instrinsic absorption of the hard and ultrahard sources (NH function) and computed the X-ray luminosity function in all bands using two methods. The first makes use of a modified version of the classic 1/Va technique, while the second performs a maximum likelihood (ML) fit using an analytic model and all available sources without binning. Results. We find that the X-ray luminosity function (XLF) is best described by a luminosity-dependent density evolution (LDDE) model. Our results show good overall agreement with previous results in the hard band, although with slightly weaker evolution. Our model in the soft band present slight discrepancies with other works in this band, the shape of our present day XLF being significantly flatter. We find faster evolution in the AGN detected in the ultrahard band than those in the hard band. Conclusions. The results reported here show that the fraction of absorbed AGN in the hard and ultrahard bands is dependent on the X-ray luminosity. We find evidence that this fraction evolves with redshift in the hard band, whereas there is none in the ultrahard band, possibly due to the low statistics. Our best-fit XLF shows that the high-luminosity AGN, detected in all bands, exhibit a similar behaviours and are fully formed earlier than the less luminous AGN. The latter sources account for the vast majority of the accretion rate and mass density of the Universe, according to an anti-hierarchical black hole growth scenario.
Cosmic time
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Constraints are found on the Galactic gamma‐ray burst luminosity function (assumed to be a truncated power law), assuming gamma‐ray bursts to be Galactic. Although most observed bursts span a narrow luminosity range, the intrinsic luminosity range can be very large. Angular isotropy additionally constrains the intrinsic luminosity range to be less than a factor of 5 for power‐law indices between −1 and 5, and requires either the maximum luminosity, the minimum luminosity, or both to be between 7.6×1041 and 1.5×1042 erg sec−1.
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Abstract We present the X-ray luminosity function (XLF) of the Antennae galaxies based on 8 observation performed with Chandra . We detect between 37 and 49 sources in each observation. After combining all observations we detect a total of 120 sources down to a limiting luminosity of ~ 2 x 10 37 erg s –1 . Comparison between the XLFs of the individual observations shows that they are not affected by source variability. The cumulative XLF of the coadded observations is well represented by a single power-law with a slope of ~ –0.5.
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Erg
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Based on a power-low spectrum of AGN γ-ray emissions,the calculation method by using the γ-ray integral photon fluxes to calculate total flux density of γ-ray,flux density at E GeV,average flux density,total luminosity,average luminosity and luminosity at E GeV were discussed,and their corresponding calculation equation were put forward.The γ-ray emission flux density,luminosity parameter etc.were calculated using those equations presented in this paper for 4 Fermi Blazars.In other bands as radio,X-ray etc.,the calculation method of flux density and luminosity can use this method too,if their emissions are power-low.
Power density
Photon flux
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The energy sources of nine infrared luminous galaxies (IRLGs) are diagnosed based on their ground-based 3-4 μm spectra. Both the equivalent width of the 3.3 μm polycyclic aromatic hydrocarbon (PAH) emission feature and the 3.3 μm PAH to far-infrared luminosity ratio (L3.3/LFIR) are analyzed. Assuming that nuclear compact starburst activity in these sources produces the 3.3 μm PAH emission as strongly as that in starburst galaxies with lower far-infrared luminosities, the following results are found. For six IRLGs, both the observed equivalent widths and the L3.3/LFIR ratios are too small to explain the bulk of their far-infrared luminosities by compact starburst activity, indicating that active galactic nucleus (AGN) activity is a dominant energy source. For the other three IRLGs, while the 3.3 μm PAH equivalent widths are within the range of starburst galaxies, the L3.3/LFIR ratios after correction for screen dust extinction are a factor of ~3 smaller. The uncertainty in the dust extinction correction factor and in the scatter of the intrinsic L3.3/LFIR ratios for starburst galaxies does not allow a determination of the ultimate energy sources for these three IRLGs.
Extinction (optical mineralogy)
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