Absolute f-values for resonance lines of neutral titanium

Bell, Graydon D.; Kalman, L. B.; Tubbs, Eldred F.

doi:10.1086/153818

Cited by 15 publications

(24 citation statements)

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“…Grevesse et al (1989) earlier produced accurate g f values by renormalising the relative oscillator strengths of Blackwell et al (1982aBlackwell et al ( ,b, 1983Blackwell et al ( , 1986c, which had been obtained by absorption spectroscopy in the Oxford furnace. As opposed to the original Oxford works, in which relative oscillator strengths were set to an absolute scale using less accurate beam-foil lifetimes from Roberts et al (1973) and the absolute data of Bell et al (1975), Grevesse et al (1989) set their new values to an absolute scale using the accurate TRLIF lifetimes of Rudolph & Helbig (1982).…”

Section: Titaniummentioning

confidence: 99%

The elemental composition of the Sun

Scott

Asplund

Grevesse

et al. 2014

A&A

269

202

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We redetermine the abundances of all iron group nuclei in the Sun, based on neutral and singly-ionised lines of Sc, Ti, V, Mn, Fe, Co and Ni in the solar spectrum. We employ a realistic 3D hydrodynamic model solar atmosphere, corrections for departures from local thermodynamic equilibrium (NLTE), stringent line selection procedures and high quality observational data. We have scoured the literature for the best quality oscillator strengths, hyperfine constants and isotopic separations available for our chosen lines. We find log Sc = 3.16 ± 0.04, log Ti = 4.93 ± 0.04, log V = 3.89 ± 0.08, log Cr = 5.62 ± 0.04, log Mn = 5.42 ± 0.04, log Fe = 7.47 ± 0.04, log Co = 4.93 ± 0.05 and log Ni = 6.20 ± 0.04. Our uncertainties factor in both statistical and systematic errors (the latter estimated for possible errors in the model atmospheres and NLTE line formation). The new abundances are generally in good agreement with the CI meteoritic abundances but with some notable exceptions. This analysis constitutes both a full exposition and a slight update of the preliminary results we presented in Asplund et al. (2009, ARA&A, 47, 481), including full line lists and details of all input data we employed.

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Section: Titaniummentioning

confidence: 99%

The elemental composition of the Sun

Scott

Asplund

Grevesse

et al. 2014

A&A

269

202

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“…Of course, the use of optical data to model the stellar parts of Malin 1 is limited. The expected stellar M/L ratio in the optical has a very large scatter (e.g., Bell & de Jong 2001;Bell et al 2003), and ideally we would prefer to have near-infrared images of Malin 1, which would provide a more accurate stellar M/L ratio.…”

Section: Modeling the Dark Matter Halomentioning

confidence: 99%

A Cosmologically Motivated Description of the Dark Matter Halo Profile for the Low Surface Brightness Galaxy, Malin 1

Seigar¹

2008

PUBL ASTRON SOC PAC

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In this paper we derive a possible mass profile for the low surface brightness galaxy, Malin 1, based upon previously published space-based and ground-based photometric properties and kinematics. We use properties of the bulge, normal disk, outer extended disk and H I mass as inputs into mass profile models. We find that the dark matter halo model of Malin 1 is best described by a halo profile that has undergone adiabatic contraction, inconsistent with the findings for most disk galaxies to date, yet consistent with rotation curve studies of M31. More importantly, we find that Malin 1 is baryon dominated in its central regions out to a radius of ∼ 10 kpc (in the bulge region). Low-surface brightness galaxies are often referred to as being dark matter dominated at all radii. If this is the case, then Malin 1 would seem to have characteristics similar to those of normal barred disk galaxies, as suggested by other recent work. We also find that Malin 1 also falls on the rotation curve shear versus spiral arm pitch angle relation for normal galaxies, although more LSB galaxies need to be studied to determine if this is typical.

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“…As input for the K-band mass-to-light ratio of the stellar populations we have adopted M K,⊙ =3.33 (Worthey 1994). It should be noticed that along with the errors in the stellar mass-to-light ratios derived here the misunderstanding of the actual IMF introduce an additional, systematic uncertainty, which, in fact, constitutes the most important source of error in the determination of the galaxy stellar mass (Bell & de Jong 2001). In addition, the poor constraints on the theoretical isochrones of upper-RGB stars and AGB stars can result in a 20 per cent uncertainty in the K-band mass-to-light ratio (Charlot et al 1996).…”

Section: Stellar Massmentioning

confidence: 99%

“…Therefore, the relative uncertainties, assuming the average absolute uncertainties given in Table 3 for ∆C n =0.07 mag, would be about 30 and 20 per cent, respectively for the nearby and intermediate-redshift galaxies. Although this still implies a significant improvement in the K-band mass-to-light ratio determination, it is also noticeable that the K filter now traces the restframe J-band luminosity, which is more affected by the misunderstanding about the actual IMF (see Bell & de Jong 2001). Finally, the J-band luminosity is also more sensitive to small differences between the assumed exponential star formation and the galaxy actual star formation history than the rest-frame K-band data.…”

Section: Stellar Massmentioning

confidence: 99%

On the Optimization of Broadband Photometry for Galaxy Evolution Studies

Paz

Madore

2002

The Astronomical Journal

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We have derived the uncertainties to be expected in the derivation of galaxy physical properties (star formation history, age, metallicity, reddening) when comparing broad-band photometry to the predictions of evolutionary synthesis models. We have obtained synthetic colors for a large sample (∼9000) of artificial galaxies assuming different star formation histories, ages, metallicities, reddening values, and redshifts. The colors derived have been perturbed by adopting different observing errors, and compared back to the evolutionary synthesis models grouped in different sets. The comparison has been performed using a combination of Monte Carlo simulations, a Maximum Likelihood Estimator and Principal Component Analysis. After comparing the input and derived output values we have been able to compute the uncertainties and covariant degeneracies between the galaxy physical properties as function of (1) the set of observables available, (2) the observing errors, and (3) the galaxy properties themselves. In this work we have considered different sets of observables, some of them including the standard Johnson/Cousins (U BV R C I C ) and Sloan Digital Sky Survey (SDSS) bands in the optical, the 2 Micron All Sky Survey (2MASS) bands in the near-infrared, and the Galaxy Evolution Explorer (GALEX) bands in the UV, at three different redshifts, z=0.0, 0.7, and 1.4. This study is intended to represent a basic tool for the design of future projects on galaxy evolution, allowing an estimate of the optimal band-pass combinations and signal-to-noise ratios required for a given scientific objective.

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Absolute f-values for resonance lines of neutral titanium

Cited by 15 publications

References 0 publications

The elemental composition of the Sun

The elemental composition of the Sun

A Cosmologically Motivated Description of the Dark Matter Halo Profile for the Low Surface Brightness Galaxy, Malin 1

On the Optimization of Broadband Photometry for Galaxy Evolution Studies

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