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22381. Transition rates on 2s2p3 configurations in N+
ID:
ivo://CDS.VizieR/J/MNRAS/462/1203
Title:
Transition rates on 2s2p3 configurations in N+
Short Name:
J/MNRAS/462/1203
Date:
21 Oct 2021
Publisher:
CDS
Description:
Wavefunctions were determined using the Multi-Configuration Dirac-Hartree-Fock (MCDHF) method. The core-core, core-valence, valence correlation, Breit interaction and quantum electrodynamics (QED) effects, as well as some higher order correlation effects, were considered to obtain accurate wavelengths (lambda), oscillator strengths (gf) and transition rates (A) of 2s^2^2p^2^-2s2p^3^, 2s2p^3^-2s^2^2pnl (n>=3) and 2s2p^3^-2s2p^2^3s E1 transitions.
22382. Transitions between Ni II bound states
ID:
ivo://CDS.VizieR/J/A+A/587/A107
Title:
Transitions between Ni II bound states
Short Name:
J/A+A/587/A107
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present rates for all E1, E2, M1, and M2 transitions among the 295 fine-structure levels of the configurations 3d^9^, 3d^8^4s, 3d^7^4s^2^, 3d^8^4p, and 3d^7^4s4p, determined through an extensive configuration interaction calculation. The CIV3 code developed by Hibbert and coworkers is used to determine for these levels configuration interaction wave functions with relativistic effects introduced through the Breit-Pauli approximation.
22383. Transitions for FeIII
ID:
ivo://CDS.VizieR/J/A+AS/116/573
Title:
Transitions for FeIII
Short Name:
J/A+AS/116/573
Date:
21 Oct 2021
Publisher:
CDS
Description:
Radiative transition probabilities have been calculated for states within the 3d6 configuration of Fe III. Magnetic dipole (M1) and electric quadrupole (E2) transition probabilities have been obtained using average energies, electrostatic and spin-orbit integrals adjusted so as to fit the observed energy levels. The most important configuration interaction (CI) and relativistic effects were included explicitly in the calculations, using the relativistic Hartree-Fock (HFR) method due to Cowan. The present work represents a refinement of previous monoconfigurational calculations of transition probabilities for forbidden lines of astrophysical interest in Fe III.
22384. Transitions in L-shell ions of Fe and Ni
ID:
ivo://CDS.VizieR/J/ApJS/156/105
Title:
Transitions in L-shell ions of Fe and Ni
Short Name:
J/ApJS/156/105
Date:
21 Oct 2021
Publisher:
CDS
Description:
Using a combined configuration interaction and many-body perturbation theory approach, we calculate the level energies of 1s^2^2l^q^ and 1s^2^2l^q-1^3l' (1<=q<=8) complexes in iron and nickel ions. Comparison of 1s^2^2l^q^ energies with experimental results shows that the calculation is accurate to within ~0.15eV for these levels. The accuracy of 1s^2^2l^q-1^3l' energies can be slightly worse, at ~0.5eV. The theoretical wavelengths of 2->3 transitions of iron ions are compared with the published experimental measurements, and discrepancies are found to be mostly within {+/-}10m{AA}. Similar accuracy is expected for wavelengths of nickel ions. Such accuracy is a significant improvement over that obtainable with standard configuration interaction methods. A complete table of 2l->3l' transition wavelengths of all L-shell ions of iron and nickel is presented.
22385. Transitions in OMC-2 FIR 4 in the far-IR
ID:
ivo://CDS.VizieR/J/A+A/556/A57
Title:
Transitions in OMC-2 FIR 4 in the far-IR
Short Name:
J/A+A/556/A57
Date:
21 Oct 2021
Publisher:
CDS
Description:
Broadband spectral surveys of protostars offer a rich view of the physical, chemical and dynamical structure and evolution of star-forming regions. The Herschel Space Observatory opened up the terahertz regime to such surveys, giving access to the fundamental transitions of many hydrides and to the high-energy transitions of many other species. A comparative analysis of the chemical inventories and physical processes and properties of protostars of various masses and evolutionary states is the goal of the Herschel CHEmical Surveys of Star forming regions (CHESS) key program. This paper focusses on the intermediate-mass protostar, OMC-2 FIR 4. We obtained a spectrum of OMC-2 FIR 4 in the 480 to 1902GHz range with the HIFI spectrometer onboard Herschel and carried out the reduction, line identification, and a broad analysis of the line profile components, excitation, and cooling. We detect 719 spectral lines from 40 species and isotopologs. The line flux is dominated by CO, H_2_O, and CH_3_OH. The line profiles are complex and vary with species and upper level energy, but clearly contain signatures from quiescent gas, a broad component likely due to an outflow, and a foreground cloud. We find abundant evidence for warm, dense gas, as well as for an outflow in the field of view. Line flux represents 2% of the 7L_{sun}_ luminosity detected with HIFI in the 480 to 1250GHz range. Of the total line flux, 60% is from CO, 13% from H_2_O and 9% from CH_3_OH. A comparison with similar HIFI spectra of other sources is set to provide much new insight into star formation regions, a case in point being a difference of two orders of magnitude in the relative contribution of sulphur oxides to the line cooling of Orion KL and OMC-2 FIR 4.
22386. Transitions of CrII
ID:
ivo://CDS.VizieR/J/A+A/511/A68
Title:
Transitions of CrII
Short Name:
J/A+A/511/A68
Date:
21 Oct 2021
Publisher:
CDS
Description:
To measure transition probabilities for CrII transitions from the z^4^H_J_, z^2^D_J_, y^4^F_J_ and y^4^G_J_ levels in the energy range 63000 to 68000cm^-1^. Radiative lifetimes were measured using time-resolved laser-induced fluorescence from a laser-produced plasma. In addition, branching fractions were determined from intensity calibrated spectra recorded with a UV Fourier transform spectrometer. The branching fractions and radiative lifetimes have been combined to yield accurate transition probabilities and oscillator strengths. We present laboratory measured transition probabilities for 145 CrII lines and radiative lifetimes for 14 CrII levels. The laboratory measured transition probabilities are compared to the values from semi-empirical calculations and laboratory measurements in the literature.
22387. Transitions of methyl formate toward Orion KL
ID:
ivo://CDS.VizieR/J/ApJ/803/97
Title:
Transitions of methyl formate toward Orion KL
Short Name:
J/ApJ/803/97
Date:
21 Oct 2021
Publisher:
CDS
Description:
We recently reported the first identification of rotational transitions of methyl formate (HCOOCH_3_) in the second torsionally excited state toward Orion Kleinmann-Low (KL), observed with the Nobeyama 45 m telescope. In combination with the identified transitions of methyl formate in the ground state and the first torsional excited state, it was found that there is a difference in rotational temperature and vibrational temperature, where the latter is higher. In this study, high spatial resolution analysis by using Atacama Large Millimeter/Submillimeter Array (ALMA) science verification data was carried out to verify and understand this difference. Toward the Compact Ridge, two different velocity components at 7.3 and 9.1 km/s were confirmed, while a single component at 7.3 km/s was identified toward the Hot Core. The intensity maps in the ground, first, and second torsional excited states have quite similar distributions. Using extensive ALMA data, we determined the rotational and vibrational temperatures for the Compact Ridge and Hot Core by the conventional rotation diagram method. The rotational temperature and vibrational temperatures agree for the Hot Core and for one component of the Compact Ridge. At the 7.3 km/s velocity component for the Compact Ridge, the rotational temperature was found to be higher than the vibrational temperature. This is different from what we obtained from the results by using the single-dish observation. The difference might be explained by the beam dilution effect of the single-dish data and/or the smaller number of observed transitions within the limited range of energy levels (<=30 K) of E_u_ in the previous study.
22388. Transitions of SI in visible and infra-red
ID:
ivo://CDS.VizieR/J/A+AS/102/435
Title:
Transitions of SI in visible and infra-red
Short Name:
J/A+AS/102/435
Date:
21 Oct 2021
Publisher:
CDS
Description:
(no description available)
22389. Transit KELT-11b observed by CHEOPS
ID:
ivo://CDS.VizieR/J/other/ExA/51.109
Title:
Transit KELT-11b observed by CHEOPS
Short Name:
J/other/ExA/51.1
Date:
21 Oct 2021
Publisher:
CDS
Description:
The CHaracterising ExOPlanet Satellite (CHEOPS) was selected on October 19, 2012, as the first small mission (S-mission) in the ESA Science Programme and successfully launched on December 18, 2019, as a secondary passenger on a Soyuz-Fregat rocket from Kourou, French Guiana. CHEOPS is a partnership between ESA and Switzerland with important contributions by ten additional ESA Member States. CHEOPS is the first mission dedicated to search for transits of exoplanets using ultrahigh precision photometry on bright stars already known to host planets. As a follow-up mission, CHEOPS is mainly dedicated to improving, whenever possible, existing radii measurements or provide first accurate measurements for a subset of those planets for which the mass has already been estimated from ground-based spectroscopic surveys. The expected photometric precision will also allow CHEOPS to go beyond measuring only transits and to follow phase curves or to search for exo-moons, for example. Finally, by unveiling transiting exoplanets with high potential for in-depth characterisation, CHEOPS will also provide prime targets for future instruments suited to the spectroscopic characterisation of exoplanetary atmospheres. To reach its science objectives, requirements on the photometric precision and stability have been derived for stars with magnitudes ranging from 6 to 12 in the V band. In particular, CHEOPS shall be able to detect Earth-size planets transiting G5 dwarf stars (stellar radius of 0.9R_sun_) in the magnitude range 6<V<9 by achieving a photometric precision of 20 ppm in 6 hours of integration time. In the case of K-type stars (stellar radius of 0.7R_{sun}_) of magnitude in the range 9<V<12, CHEOPS shall be able to detect transiting Neptune-size planets achieving a photometric precision of 85ppm in 3 hours of integration time. This precision has to be maintained over continuous periods of observation for up to 48 hours. This precision and stability will be achieved by using a single, frame-transfer, back-illuminated CCD detector at the focal plane assembly of a 33.5cm diameter, on-axis Ritchey-Chretien telescope. The nearly 275kg spacecraft is nadir-locked, with a pointing accuracy of about 1arcsec rms, and will allow for at least 1Gbit/day downlink. The sun-synchronous dusk-dawn orbit at 700km altitude enables having the Sun permanently on the backside of the spacecraft thus minimising Earth stray light. A mission duration of 3.5 years in orbit is foreseen to enable the execution of the science programme. During this period, 20% of the observing time is available to the wider community through yearly ESA call for proposals, as well as through discretionary time approved by ESA's Director of Science. At the time of this writing, CHEOPS commissioning has been completed and CHEOPS has been shown to fulfill all its requirements. The mission has now started the execution of its science programme.
22390. Transit light curves of GJ1214
ID:
ivo://CDS.VizieR/J/ApJ/736/12
Title:
Transit light curves of GJ1214
Short Name:
J/ApJ/736/12
Date:
21 Oct 2021
Publisher:
CDS
Description:
The super-Earth GJ1214b transits a nearby M dwarf that exhibits a 1% intrinsic variability in the near-infrared. Here, we analyze new observations to refine the physical properties of both the star and planet. We present three years of out-of-transit photometric monitoring of the stellar host GJ1214 from the MEarth Observatory and find the rotation period to be long, most likely an integer multiple of 53 days, suggesting low levels of magnetic activity and an old age for the system. We show that such variability will not pose significant problems to ongoing studies of the planet's atmosphere with transmission spectroscopy. We analyze two high-precision transit light curves from ESO's Very Large Telescope (VLT) along with seven others from the MEarth and Fred Lawrence Whipple Observatory 1.2m telescopes, finding physical parameters for the planet that are consistent with previous work. The VLT light curves show tentative evidence for spot occultations during transit. Using two years of MEarth light curves, we place limits on additional transiting planets around GJ1214 with periods out to the habitable zone of the system. We also improve upon the previous photographic V-band estimate for the star, finding V=14.71+/-0.03.

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