The luminosity function of narrow-line Seyfert 1 galaxies based on SDSS data (DR7)

Ermash, A. A.

doi:10.1134/s106377291305003x

Cited by 5 publications

(7 citation statements)

References 29 publications

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“…In order to check our results the same calculations were performed also for N ≥ 50. The results obtained are identical except that errors are lower (there are more objects for each density bin) and uncertainties in ρ are The same interval in AGN luminosity as for calculation of luminosity function [1] was used. But it was split in 4 intervals instead of 12: 5.25 -6.25, 6.25 -7.0, 7.0 -7.75, 7.75 -9.0.…”

Section: Spatial Density Of Agn and The Large-scale Structurementioning

confidence: 90%

“…In our previous work [1] we have obtained the luminosity function of NLS in [OIII]λ5007Å. This forbidden line is emitted at large distance from the active nuclei in NLR, which has conical geometry, thus this line does not suffer from orientation effects and obscuration.…”

Section: Intoductionmentioning

confidence: 99%

“…This approach allows us to normalize sample of considered objects to uniform complete sample of galaxies which traces variations of density of the Universe. For details see [1]. 1 Low-Ionization Nuclei Emission Region galaxies.…”

Section: Intoductionmentioning

confidence: 99%

“…For the redshift interval considered this is correct. For details see [1]. Hence, normalized amount of AGN is…”

Section: Data Processingmentioning

confidence: 99%

“…). Details see in [1]. Then we have split the considered volume of the Universe into elements limited by redshift (z i < z < z i+1 ), ascension and declination (α min,j < α < α max,j ; δ min,j < δ < δ max,j ).…”

Section: Now We Can Obtainmentioning

confidence: 99%

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Narrow-line Seyfert Galaxies. Connection between abundance and the large-scale structure

Ermash

Komberg

2014

J. Phys.: Conf. Ser.

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In this work the correlations between spatial concentrations of active nuclei (NLS and BLS) and concentration of galaxies of full uniform sample were obtained. Methods, developed by the author in previous paper [1] were used. Galaxies of this uniform sample trace the large-scale structure. We used SDSS DR 7 data. The correlations obtained are linear and the NLS/BLS ratio is constant. That leads to conclusion that amounts NLS and BLS are some fixed fraction of all galaxies independent on the density of large-scale environment. In order to check validity of our results were also confirmed the well known result that fraction of red galaxies increases with density of environment. Also it was confirmed that this trend is more prominent for less massive galaxies.

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Section: Spatial Density Of Agn and The Large-scale Structurementioning

confidence: 90%

Section: Intoductionmentioning

confidence: 99%

Section: Intoductionmentioning

confidence: 99%

“…For the redshift interval considered this is correct. For details see [1]. Hence, normalized amount of AGN is…”

Section: Data Processingmentioning

confidence: 99%

Section: Now We Can Obtainmentioning

confidence: 99%

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Narrow-line Seyfert Galaxies. Connection between abundance and the large-scale structure

Ermash

Komberg

2014

J. Phys.: Conf. Ser.

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Characterizing the ELG luminosity functions in the nearby Universe

Favole,

Gonzalez-Perez,

Ascasibar

et al. 2024

A&A

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Nebular emission lines are powerful diagnostics for the physical processes at play in galaxy formation and evolution. Moreover, emission-line galaxies (ELGs) are one of the main targets of current and forthcoming spectroscopic cosmological surveys. We investigate the contributions to the line luminosity functions (LFs) of different galaxy populations in the local Universe, providing a benchmark for future surveys of earlier cosmic epochs. The large statistics of the observations from the SDSS DR7 main galaxy sample and the MPA-JHU spectral catalog enabled us to precisely measure the and, for the first time, the and emission-line LFs over $ Gyrs in the low-$z$ Universe, $0.02<z<0.22$. We present a generalized max $ LF estimator capable of simultaneously correcting for spectroscopic, $r-$band magnitude, and emission-line incompleteness. We studied the contribution to the LF of different types of ELGs classified using two methods: (i) the value of the specific star formation rate (sSFR), and (ii) the line ratios on the Baldwin--Phillips--Terlevich (BPT) and the WHAN (i.e. equivalent width H alpha $, versus the line ratio) diagrams. The ELGs in our sample are mostly star forming, with $84$ percent having $ sSFR $. When classifying ELGs using the BPT+WHAN diagrams, we find that $63.3$ percent are star forming, only $0.03$ are passively evolving, and $1.3$ have nuclear activity (Seyfert). The rest are low-ionization narrow emission-line regions (LINERs) and composite ELGs. We found that a Saunders function is the most appropriate to describe all of the emission-line LFs, both observed and dust-extinction-corrected (i.e., intrinsic). They are dominated by star-forming regions, except for the bright end of the and LFs (i.e. NII $, $L_ OIII $), where the contribution of Seyfert galaxies is not negligible. In addition to the star-forming population, composite galaxies and LINERs are the ones that contribute the most to the ELG numbers at $L < 10^ $. We do not observe significant evolution with redshift of our ELGs at $0.02<z<0.22$. All of our results, including data points and analytical fits, are publicly available. Local ELGs are dominated by star-forming galaxies, except for the brightest $ NII $ and $ OIII $ emitters, which have a large contribution of Seyfert galaxies. The local line luminosity functions are best described by Saunders functions. We expect these two conclusions to hold up at higher redshifts for the ELG targeted by current cosmological surveys, such as DESI and Euclid.

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Narrow-line Seyfert 1 galaxies. Relationship between their frequency of occurrence and the large-scale structure of the universe

Ermash

2014

Astron. Rep.

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The luminosity function of narrow-line Seyfert 1 galaxies based on SDSS data (DR7)

Cited by 5 publications

References 29 publications

Narrow-line Seyfert Galaxies. Connection between abundance and the large-scale structure

Narrow-line Seyfert Galaxies. Connection between abundance and the large-scale structure

Characterizing the ELG luminosity functions in the nearby Universe

Narrow-line Seyfert 1 galaxies. Relationship between their frequency of occurrence and the large-scale structure of the universe

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