PyNeb: a new tool for analyzing emission lines

Luridiana, V.; Morisset, Charles; Shaw, Richard A.

doi:10.1051/0004-6361/201323152

Cited by 481 publications

(425 citation statements)

References 52 publications

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“…Table 2. The list of emission lines searched for in the spectra, with wavelengths collected from Luridiana, Morisset & Shaw (2015). We split the lines into collisional and recombination groups.…”

Section: From Spectra To Emission Line Cataloguesmentioning

confidence: 99%

The evolution of the [O ii], H β and [O iii] emission line luminosity functions over the last nine billions years

Comparat

Zhu

González-Pérez

et al. 2016

Mon. Not. R. Astron. Soc.

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Citation for published item:gomp r tD tF nd huD qF nd qonz lezE erezD F nd xor ergD F nd xewm nD tF nd resseD vF nd i h rdD tF nd epesD qF nd unei D tFE F nd i hoorD eF nd r d D pF nd w r stonD gF nd e heD gF nd helu D F nd tulloD iF @PHITA 9 he evolution of the y ss D r nd y sss emission line luminosity fun tions over the l st nine illions ye rsF9D wonthly noti es of the oy l estronomi l o ietyFD RTI @IAF ppF IHUTEIHVUF Further information on publisher's website: Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTEmission line galaxies are one of the main tracers of the large-scale structure to be targeted by the next-generation dark energy surveys. To provide a better understanding of the properties and statistics of these galaxies, we have collected spectroscopic data from the VVDS and DEEP2 deep surveys and estimated the galaxy luminosity functions (LFs) of three distinct emission lines, [O II] (λλ3726, 3729) (0.5 < z < 1.3), Hβ (λ4861) (0.3 < z < 0.8) and [O III] (λ5007) (0.3 < z < 0.8). Our measurements are based on 35 639 emission line galaxies and cover a volume of ∼10 7 Mpc 3 . We present the first measurement of the Hβ LF at these redshifts. We have also compiled LFs from the literature that were based on independent data or covered different redshift ranges, and we fit the entire set over the whole redshift range with analytic Schechter and Saunders models, assuming a natural redshift dependence of the parameters. We find that the characteristic luminosity (L * ) and density (φ * ) of all LFs increase with redshift. Using the Schechter model over the redshift ranges considered, we find that, for [O II] emitters, the characteristic luminosity L * (z = 0.5) = 3.2 × 10 41 erg s −1 increases by a factor of 2.7 ± 0.2 from z = 0.5 to 1.3; for Hβ emitters L * (z = 0.3) = 1.3 × 10 41 erg s −1 increases by a factor of 2.0 ± 0.2 from z = 0.3 to 0.8; and for [O III] emitters L * (z = 0.3) = 7.3 × 10 41 erg s −1 increases by a factor of 3.5 ± 0.4 from z = 0.3 to 0.8.

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Section: From Spectra To Emission Line Cataloguesmentioning

confidence: 99%

The evolution of the [O ii], H β and [O iii] emission line luminosity functions over the last nine billions years

Comparat

Zhu

González-Pérez

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Table 2 of ). Physical conditions and ionic abundances were computed using PN, a new python-based code for the analysis of nebular data (Luridiana et al 2015). The atomic data set used is listed in Tables A.2 and 4).…”

Section: The True Nature Of Objects Observed With Gtcmentioning

confidence: 99%

The planetary nebulae and H II regions in NGC 6822 revisited. Clues to AGB nucleosynthesis

García‐Rojas

Peña

Flores-Durán

et al. 2016

A&A

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Aims. The chemical behaviour of an ample sample of planetary nebulae (PNe) in NGC 6822 is analysed.Methods. Spectrophotometric data of 11 PNe and two H  regions were obtained with the OSIRIS spectrograph attached to the Gran Telescopio Canarias. Data for other 13 PNe and three H  regions were retrieved from the literature. Physical conditions and chemical abundances of O, N, Ne, Ar, and S were derived in a consistent way for 19 PNe and 4 H  regions.Results. Abundances in the PNe sample are widely distributed showing 12 + log (O/H) from 7.4 to 8.2 and 12 + log (Ar/H) from 4.97 to 5.80. Two groups of PNe can be differentiated: one old with low metallicity (12 + log (O/H) < 8.0 and 12 + log (Ar/H) < 5.7) and another younger one with metallicities similar to the values for H  regions. The old objects are distributed in a larger volume than the young ones. An important fraction of PNe (over 30%) was found to be highly N-rich (Peimbert Type I PNe). Such PNe occur at any metallicity. In addition, about 60% of the sample presents high ionization (He ++ /He ≥ 0.1), possessing a central star with effective temperature higher than 100 000 K. Possible biases in the sample are discussed. From comparison with stellar evolution models by Karakas (2010) and Fishlock et al. (2014) of the observed N/O abundance ratios, our PNe should have had initial masses that are lower than 4 M , although if the comparison is made with Ne vs. O abundances, the initial masses should have been lower than 2 M . It appears that these models of stars of 2−3 M are producing too much 22 Ne in the stellar surface at the end of the AGB. On the other hand, the comparison with another set of stellar evolution models with a different treatment of convection and on the assumptions about the overshoot of the convective core during the core H-burning phase, provided there is reasonable agreement between the observed and predicted N/O and Ne/H ratios if initial masses of more massive stars are about 4 M .

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“…The computations of physical conditions were carried out with PyNeb v1.0.9 (Luridiana et al 2015), a python-based package dedicated to the analysis of emission line spectra. The methodology followed for the derivation of the electron density, n e , and the electron temperature, T e , has been described in previous papers of our group.…”

Section: Physical Conditionsmentioning

confidence: 99%

s-process enrichment in the planetary nebula NGC 3918. Results from deep echelle spectrophotometry

García‐Rojas¹,

Madonna²,

Luridiana³

et al. 2015

Mon. Not. R. Astron. Soc.

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The chemical content of the planetary nebula NGC 3918 is investigated through deep, highresolution (R∼40000) UVES at VLT spectrophotometric data. We identify and measure more than 750 emission lines, making ours one of the deepest spectra ever taken for a planetary nebula. Among these lines we detect very faint lines of several neutron-capture elements (Se, Kr, Rb, and Xe), which enable us to compute their chemical abundances with unprecedented accuracy, thus constraining the efficiency of the s-process and convective dredge-up in NGC 3918s progenitor star. We find that Kr is strongly enriched in NGC 3918 and that Se is less enriched than Kr, in agreement with the results of previous papers and with predicted s-process nucleosynthesis. We also find that Xe is not as enriched by the s-process in NGC 3918 as is Kr and, therefore, that neutron exposure is typical of modestly subsolar metallicity AGB stars. A clear correlation is found when representing [Kr/O] vs. log(C/O) for NGC 3918 and other objects with detection of multiple ions of Kr in optical data, confirming that carbon is brought to the surface of AGB stars along with s-processed material during third dredge-up episodes, as predicted by nucleosynthesis models. We also detect numerous refractory element lines (Ca, K, Cr, Mn, Fe, Co, Ni, and Cu) and a large number of metal recombination lines of C, N, O, and Ne. We compute physical conditions from a large number of diagnostics, which are highly consistent among themselves assuming a three-zone ionization scheme. Thanks to the high ionization of NGC 3918 we detect a large number of recombination lines of multiple ionization stages of C, N, O and Ne. The abundances obtained for these elements by using recently-determined state-of-the-art ICF schemes or simply adding ionic abundances are in very good agreement, demonstrating the quality of the recent ICF scheme for high ionization planetary nebulae.

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PyNeb: a new tool for analyzing emission lines

Cited by 481 publications

References 52 publications

The evolution of the [O ii], H β and [O iii] emission line luminosity functions over the last nine billions years

The evolution of the [O ii], H β and [O iii] emission line luminosity functions over the last nine billions years

The planetary nebulae and H II regions in NGC 6822 revisited. Clues to AGB nucleosynthesis

s-process enrichment in the planetary nebula NGC 3918. Results from deep echelle spectrophotometry

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