The ratio of optical to infrared emission-line strengths in O III as electron temperature diagnostics for planetary nebulae

1990 ◽  
Vol 350 ◽  
pp. 262 ◽  
Author(s):  
F. P. Keenan ◽  
K. M. Aggarwal
Keyword(s):  
Emission Line ◽  
Electron Temperature ◽  
Planetary Nebulae ◽  
Infrared Emission ◽  
Temperature Diagnostics ◽  
Line Strengths

The 1 1S-n 1 P/1 1S-2 1 P emission-line ratios in SI XIII as electron temperature diagnostics for solar flares and active regions

1990 ◽  
Vol 363 ◽  
pp. 310 ◽  
Author(s):  
F. P. Keenan ◽  
S. M. McCann ◽  
K. J. H. Phillips
Keyword(s):  
Emission Line ◽  
Electron Temperature ◽  
Solar Flares ◽  
Active Regions ◽  
Temperature Diagnostics

scholarly journals Abundances of Iron-Group Elements in Planetary Nebulae and Consequences for Chemical Enrichment

2016 ◽  
Vol 12 (S323) ◽  
pp. 82-85
Author(s):  
Harriet L. Dinerstein ◽  
T. R. Geballe ◽  
N. C. Sterling
Keyword(s):  
Emission Line ◽  
Chemical Evolution ◽  
Planetary Nebulae ◽  
Infrared Emission ◽  
Thick Disk ◽  
Galactic Chemical Evolution ◽  
Iron Group ◽  
Chemical Enrichment ◽  
Group Species

AbstractWe have developed a method for determining elemental Fe-group abundances in planetary nebulae using an infrared emission line of Zn, the least refractory Fe-group species. Many planetary nebulae, particularly those of the Milky Way’s thick disk and bulge, display subsolar [Fe/H] (as inferred from Zn) although their abundances of α elements such as O, S, and Ar are nearly solar. We discuss the implications for determining enhancements of species synthesized by the progenitor star during the AGB (e.g.,s-process products), and for galactic chemical evolution in view of the metallicity dependence of AGB nucleosynthetic yields.

Fe XXI emission line ratios as electron temperature diagnostics for the coronae of cool stars

Solar Physics ◽  
1996 ◽  
Vol 169 (1) ◽  
pp. 47-53 ◽  
Author(s):  
F. P. Keenan ◽  
V. J. Foster ◽  
K. M. Aggarwal ◽  
K. G. Widing
Keyword(s):  
Emission Line ◽  
Electron Temperature ◽  
Cool Stars ◽  
Temperature Diagnostics

X-ray emission-line ratios in MG XI as electron temperature diagnostics for solar flares and active regions

1992 ◽  
Vol 393 ◽  
pp. 815 ◽  
Author(s):  
F. P. Keenan ◽  
K. J. H. Phillips ◽  
L. K. Harra ◽  
E. S. Conlon ◽  
A. E. Kingston
Keyword(s):  
Emission Line ◽  
Electron Temperature ◽  
Solar Flares ◽  
Active Regions ◽  
X Ray ◽  
Temperature Diagnostics

scholarly journals The SAMI Galaxy Survey: reconciling strong emission line metallicity diagnostics using metallicity gradients

2021 ◽  
Vol 502 (3) ◽  
pp. 3357-3373
Author(s):  
Henry Poetrodjojo ◽  
Brent Groves ◽  
Lisa J Kewley ◽  
Sarah M Sweet ◽  
Sebastian F Sanchez ◽  
...  
Keyword(s):  
Emission Line ◽  
Electron Temperature ◽  
Gas Phase ◽  
Mass Range ◽  
Accurate Method ◽  
Emission Lines ◽  
Mass Relation ◽  
Strong Emission ◽  
Data Release ◽  
Accurate Comparison

ABSTRACT We measure the gas-phase metallicity gradients of 248 galaxies selected from Data Release 2 of the SAMI Galaxy Survey. We demonstrate that there are large systematic discrepancies between the metallicity gradients derived using common strong emission line metallicity diagnostics. We determine which pairs of diagnostics have Spearman’s rank coefficients greater than 0.6 and provide linear conversions to allow the accurate comparison of metallicity gradients derived using different strong emission line diagnostics. For galaxies within the mass range 8.5 < log (M/M⊙) < 11.0, we find discrepancies of up to 0.11 dex/Re between seven popular diagnostics in the metallicity gradient–mass relation. We find a suggestion of a break in the metallicity gradient–mass relation, where the slope shifts from negative to positive, occurs between 9.5 < log (M/M⊙) < 10.5 for the seven chosen diagnostics. Applying our conversions to the metallicity gradient–mass relation, we reduce the maximum dispersion from 0.11 dex/Re to 0.02 dex/Re. These conversions provide the most accurate method of converting metallicity gradients when key emission lines are unavailable. We find that diagnostics that share common sets of emission line ratios agree best, and that diagnostics calibrated through the electron temperature provide more consistent results compared to those calibrated through photoionization models.

scholarly journals Exploring the link between C IV outflow kinematics and sublimation-temperature dust in quasars

2020 ◽  
Author(s):  
Matthew J Temple ◽  
Manda Banerji ◽  
Paul C Hewett ◽  
Amy L Rankine ◽  
Gordon T Richards
Keyword(s):  
Emission Line ◽  
High Frequency ◽  
Infrared Emission ◽  
Black Hole Mass ◽  
Sublimation Temperature ◽  
Continuum Source ◽  
Broad Emission ◽  
Line Region ◽  
Using Data

Abstract Using data from SDSS, UKIDSS and WISE, we investigate the properties of the high-frequency cutoff to the infrared emission in ≃5000 carefully selected luminous (Lbol ∼ 1047) type 1 quasars. The strength of ≃2 μm emission, corresponding to emission from the hottest ($T>1200\rm \, K$) dust in the sublimation zone surrounding the central continuum source, is observed to correlate with the blueshift of the C iv λ1550 emission line. We therefore find that objects with stronger signatures of nuclear outflows tend to have a larger covering fraction of sublimation-temperature dust. When controlling for the observed outflow strength, the hot dust covering fraction does not vary significantly across our sample as a function of luminosity, black hole mass or Eddington fraction. The correlation between the hot dust and the C iv line blueshifts, together with the lack of correlation between the hot dust and other parameters, therefore provides evidence of a link between the properties of the broad emission line region and the infrared-emitting dusty regions in quasars.

scholarly journals Hybrid 3-D Spectrophotometry of Emission-Line Nebulae at Ohio State

1995 ◽  
Vol 149 ◽  
pp. 167-171
Author(s):  
Richard W. Pogge ◽  
Nancy Joanne Lame
Keyword(s):  
Emission Line ◽  
Planetary Nebulae ◽  
Hii Regions ◽  
Ohio State University ◽  
State University ◽  
Considerable Success ◽  
Fabry Perot ◽  
The Ohio State University ◽  
Scientific Results ◽  
Narrowband Filter

AbstractA program of 3-D spectrophotometry of emission nebulae being carried out at the Ohio State University will be described. We have had considerable success combining Fabry-Perot imaging, long-slit spectroscopy, and narrowband filter imaging into a hybrid 3-D spectroscopic approach that we have used to obtain detailed spectrophotometric maps of the density, temperature, extinction, and ionization in HII regions and Planetary Nebulae. The centerpiece instrument of this effort, the OSU Imaging Fabry-Perot Spectrograph (IFPS), will be described, and scientific results illustrative of our work will be presented.

Relative quasar luminosities determined from emission line strengths

Nature ◽  
1978 ◽  
Vol 273 (5662) ◽  
pp. 431-435 ◽  
Author(s):  
Jack A. Baldwin ◽  
William L. Burke ◽  
C. Martin Gaskell ◽  
E. J. Wampler
Keyword(s):  
Emission Line ◽  
Line Strengths
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