Error in Attribution of Data Source of a Cited Study in the Article by Bruderer et al (Arthritis Rheumatol, January 2014)

Bruderer, Saskia Gabriela; Bodmer, Michael; Jick, Susan S.; Meier, Christoph

doi:10.1002/art.38364

Cited by 2 publications

(4 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The foreground absorption line width (equivalent width is 3.2 km s −1 ) is clearly larger than the corresponding feature in the CO lines (∆v = 0.8 km s −1 ; Van der Wiel 2011), and more comparable to the width of the feature seen in CH (∆v = 1.8 km s −1 , Bruderer et al 2010). Using the line width of CH as the ∆v caused by Doppler broadening for HF, and fitting the absorption feature using equations ( 1) and ( 2), leads to a minimum optical depth of eight, and thus a minimum HF column density of 4 • 10 13 cm −2 in the foreground cloud.…”

Section: Afgl 2591mentioning

confidence: 84%

Hydrogen Fluoride in High-Mass Star-Forming Regions

Emprechtinger

Monje

Tak

et al. 2012

ApJ

View full text Add to dashboard Cite

Hydrogen fluoride has been established to be an excellent tracer of molecular hydrogen in diffuse clouds. In denser environments, however, the HF abundance has been shown to be approximately two orders of magnitude lower. We present Herschel/HIFI observations of HF J = 1−0 toward two high-mass star formation sites, NGC6334 I and AFGL 2591. In NGC6334 I the HF line is seen in absorption in foreground clouds and the source itself, while in AFGL 2591 HF is partially in emission. We find an HF abundance with respect to H 2 of 1.5 · 10 −8 in the diffuse foreground clouds, whereas in the denser parts of NGC6334 I, we derive a lower limit on the HF abundance of 5 · 10 −10 . Lower HF abundances in dense clouds are most likely caused by freeze out of HF molecules onto dust grains in highdensity gas. In AFGL 2591, the view of the hot core is obstructed by absorption in the massive outflow, in which HF is also very abundant (3.6 · 10 −8 ) due to the desorption by sputtering. These observations provide further evidence that the chemistry of interstellar fluorine is controlled by freeze out onto gas grains.

show abstract

Section: Afgl 2591mentioning

confidence: 84%

Hydrogen Fluoride in High-Mass Star-Forming Regions

Emprechtinger

Monje

Tak

et al. 2012

ApJ

View full text Add to dashboard Cite

show abstract

“…The following describes the general scheme of the proposed calibration system. Features of possible implementations of the method is provided in Appendix A, while details of a specific implementation of this method to the Dark Energy Survey experiment [19] will be describe in a future paper [20]. Figure 1 summarises a system-level scheme for building the calibrating process to measure the weak lensing signal of galaxies with high precision.…”

Section: A Way Forwardmentioning

confidence: 99%

Section: A Way Forwardmentioning

confidence: 99%

See 1 more Smart Citation

A way forward for Cosmic Shear: Monte-Carlo Control Loops

Réfrégier

Amara

2014

Physics of the Dark Universe

View full text Add to dashboard Cite

Weak lensing by large scale structure or 'cosmic shear' is a potentially powerful cosmological probe to shed new light on Dark Matter, Dark Energy and Modified Gravity. It is based on the weak distortions induced by large-scale structures on the observed shapes of distant galaxies through gravitational lensing. While the potentials of this purely gravitational effect are great, results from this technique have been hampered because the measurement of this weak effect is difficult and limited by systematics effects. In particular, a demanding step is the measurement of the weak lensing shear from wide field CCD images of galaxies. We describe the origin of the problem and propose a way forward for cosmic shear. Our proposed approach is based on Monte-Carlo Control Loops and draws upon methods widely used in particle physics and engineering. We describe the control loop scheme and show how it provides a calibration method based on fast image simulations tuned to reproduce the statistical properties of a specific cosmic shear data set. Through a series of iterative loops and diagnostic tests, the Monte Carlo image simulations are made robust to perturbations on modeling input parameters and thus to systematic effects. We discuss how this approach can make the problem tractable and unleash to full potential of cosmic shear for cosmology.

show abstract

Error in Attribution of Data Source of a Cited Study in the Article by Bruderer et al (Arthritis Rheumatol, January 2014)

Cited by 2 publications

References 0 publications

Hydrogen Fluoride in High-Mass Star-Forming Regions

Hydrogen Fluoride in High-Mass Star-Forming Regions

A way forward for Cosmic Shear: Monte-Carlo Control Loops

Contact Info

Product

Resources

About