Erratum: “The Swan System of C
                    <sub>2</sub>
                    : A Global Analysis of Fourier Transform Emission Spectra” (ApJS, 169, 472 [2007])

Tanabashi, Akihiro; Hirao, T.; Bernath, Peter F.

doi:10.1086/518694

Cited by 12 publications

(20 citation statements)

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“…Atomic lines were taken from the latest Kurucz line lists 2 and the CN line list described in Meléndez & Barbuy (1999) was adopted. The line list for the 0-1 and 1-2 bands of the C 2 Swan system was constructed in a similar way to the 0-0 band described in Meléndez & Cohen (2007), but with the line positions taken primarily from Tanabashi et al (2007) and complemented with Phillips & Davis (1968) data for the higher excitation lines not included by Tanahashi et al. Relative oscillator strengths for the 0-1 and 1-2 bands were taken from Kokkin et al (2007), normalizing those values to the laboratory oscillator strength of the 0-0 band recommended by Grevesse et al (1991), f 00 = 3.03 × 10 −2 .…”

Section: Discussionmentioning

confidence: 99%

Another forbidden solar oxygen abundance: the [O I] 5577 Å line

Meléndez

Asplund

2008

A&A

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Context. Recent works with improved model atmospheres, line formation, atomic and molecular data, and detailed treatment of blends have resulted in a significant downward revision of the solar oxygen abundance. Conclusions. The oxygen abundance derived here is close to the 3D-based estimates from the two other [O i] lines at 6300 and 6363 Å, the permitted O i lines and vibrational and rotational OH transitions in the infrared. Our study thus supports a low solar oxygen abundance (log O ≈ 8.7), independent of the adopted model atmosphere.

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Section: Discussionmentioning

confidence: 99%

Another forbidden solar oxygen abundance: the [O I] 5577 Å line

Meléndez

Asplund

2008

A&A

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“…4, the SDSS spectra of four peculiar DQ WDs are shown to illustrate the effect. The bandheads of the usually strongest sequences of C 2 bands (Tanabashi et al 2007) were over-plotted as vertical red dashed lines and those from the red CN bands (Davis et al 1987) as magenta lines. The downscaled sky spectrum is over-plotted in green at the bottom of each panel.…”

Section: Uncertain Classifications and Possible Contaminationmentioning

confidence: 99%

Broad-band spectral energy distribution of 3000 Å break quasars from the Sloan Digital Sky Survey

Meusinger

Schalldach

Mirhosseini

et al. 2016

A&A

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Context. In past decades, huge surveys have confirmed the existence of populations of exotic and hitherto unknown quasar types. The discovery and investigation of these rare peculiar objects is important because they may represent links to special evolutionary stages and hold clues to the evolution of quasars and galaxies. Aims. The Sloan Digital Sky Survey (SDSS) discovered the unusual quasars J010540.75-003313.9 and J220445.27+003141.8 and a small number of similar objects. Their spectra are characterised by a break in the continuum around 3000 Å that neither shows the typical structure of broad absorption line (BAL) troughs nor is explained by typical intrinsic dust reddening. The main aim of the present paper was twofold. First, a new target-oriented search was performed in the spectra database of the SDSS to construct a sizable sample of such 3000 Å break quasars. Second, their broad-band spectral energy distribution (SED) was compared with SEDs of BAL quasars. Methods. We used the method of Kohonen self-organising maps for data mining in the SDSS spectra archive to search for more quasars with properties comparable to the prototypes J010540.75-003313.9 and J220445.27+003141.8. We constructed a sample of 3000 Å break quasars and comparison samples of quasars with similar properties, to some extent, but also showing indications for typical BAL features. Particular attention was payed to a possible contamination by rare stellar spectral types, in particular DQ white dwarfs. We construct ensemble-averaged broad-band SEDs based on archival data from SDSS, GALEX, 2MASS, UKIDSS, WISE, and other surveys. The SEDs were corrected for dust absorption at the systemic redshifts of the quasars by the comparison with the average SED of normal quasars. Results. We compiled a list of 23 quasars classified as 3000 Å break quasars with properties similar to 010540.75-003313.9 and J220445.27+003141.8. Their de-reddened arithmetic median composite SED is indistinguishable from that of the unusual BAL quasars. We conclude that 3000 Å break quasars are most likely extreme versions of BAL quasars. Assuming that the intrinsic SED of the continuum source is represented by the quasar composite SED, the 3000 Å break quasars tend to be intrinsically more luminous than ordinary quasars.

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“…For both states (a 3 Π u and d 3 Π g ) the energy levels were computed in a first step from the formulae and constants provided by Phillips (1968) with T v values from Tanabashi et al (2007) (their Tables 3 and 4). We computed all energy values for the vibrational quantum number v ≤ 5 and rotational quantum number N ≤ 100.…”

Section: Model For Thementioning

confidence: 99%

“…The F(J) values were computed from the formulae and constants provided by Phillips (1968) for the 12 C 2 radical, in which the constants were adapted to 12 C 13 C according to the formulae given by Herzberg (1950). The T e and G(v) values were taken from Tanabashi et al (2007) and were also adapted to 12 C 13 C for G(v). We write (Herzberg 1950)…”

Section: Modeling Thementioning

confidence: 99%

The¹²C₂/¹²C¹³C isotopic ratio in comets C/2001 Q4 (NEAT) and C/2002 T7 (LINEAR)

Rousselot¹,

Jehin²,

Manfroid³

et al. 2012

A&A

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Context. Measuring the carbon isotope abundance ratio in comets allows one to constrain the conditions in the outer protosolar nebula. Different measurements of the 12 C/ 13 C ratio, using various molecules, have already been published for different solar system objects, such as the Sun, the Earth, the Moon, asteroids, planets, or comets. So far, all these measurements are consistent with 12 C/ 13 C ∼ 90, but significant differences have been observed. This ratio is remarkably constant in comets (91.0 ± 3.6) for studies based on the CN radical, but it presents stronger variations in studies based on other radicals. Aims. This paper aims at measuring the 12 C/ 13 C ratio in two bright Oort cloud comets using the 12 C 2 and 12 C 13 C emission lines and an improved method. The ratios will be compared to those obtained for the same comets with another radical, CN. Methods. We used the (2, 1) and (1, 0) bandheads of the 12 C 13 C, near 4723 and 4745 Å to measure the 12 C/ 13 C ratio and compared their intensity to the 12 C 2 lines of the same bands. We developed a model for interpreting observational data obtained at high resolution (∼70 000) using the 8.

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Erratum: “The Swan System of C ₂ : A Global Analysis of Fourier Transform Emission Spectra” (ApJS, 169, 472 [2007])

Cited by 12 publications

References 0 publications

Another forbidden solar oxygen abundance: the [O I] 5577 Å line

Another forbidden solar oxygen abundance: the [O I] 5577 Å line

Broad-band spectral energy distribution of 3000 Å break quasars from the Sloan Digital Sky Survey

The¹²C₂/¹²C¹³C isotopic ratio in comets C/2001 Q4 (NEAT) and C/2002 T7 (LINEAR)

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Erratum: “The Swan System of C 2 : A Global Analysis of Fourier Transform Emission Spectra” (ApJS, 169, 472 [2007])

Cited by 12 publications

References 0 publications

Another forbidden solar oxygen abundance: the [O I] 5577 Å line

Another forbidden solar oxygen abundance: the [O I] 5577 Å line

Broad-band spectral energy distribution of 3000 Å break quasars from the Sloan Digital Sky Survey

The12C2/12C13C isotopic ratio in comets C/2001 Q4 (NEAT) and C/2002 T7 (LINEAR)

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Erratum: “The Swan System of C ₂ : A Global Analysis of Fourier Transform Emission Spectra” (ApJS, 169, 472 [2007])

The¹²C₂/¹²C¹³C isotopic ratio in comets C/2001 Q4 (NEAT) and C/2002 T7 (LINEAR)