Artiklen identificerer de institutionelle mekanismer, som har skabt og vedligeholdt den overraskende høje politiske opbakning, som har kendetegnet den aktivistiske udenrigspolitiks to flagskibe i ...næsten 60 år: de internationale militære operationer og udviklingsbistanden. Den høje og konstante opbakning skyldes to policy-fællesskaber, der inddrager de centrale aktører og anvender standard- og krisestyringsprocedurer i form af ekspertudredninger, kommissioner, flerårige budgetaftaler, konsultationer, politiske forlig og strategier til at skabe kompromiser på de to policy-områder. Den høje politiske opbakning understøttes af manglende folkelig interesse for de to områder og behovet for at fremstå som en troværdig international samarbejdspartner. Nøglen til at forstå den udenrigspolitiske aktivismes fremtidige udvikling ligger derfor ikke i udlandet eller i meningsmålingerne, som det normalt antages. Den ligger på Slotsholmen.
This article identifies the institutional mechanisms that have created and sustained the surprisingly high level of political support that has characterized the two flagships of the activist Danish ...foreign policy for nearly 60 years: international military operations and development assistance. The high support results from two policy communities involving the key actors and using standard- and crisis-management procedures in the form of white papers, commissions, multi-year budget agreements, consultation, political agreements and strategies to build compromises within the two policy-areas. The high level of political support is underpinned by public disinterest in the two areas and the need to establish an international reputation as a reliable partner. The key to understanding the future of Denmark’s activist foreign policy consequently does not lie abroad or in opinion polls as it is generally assumed. It lies in the Danish parliament and the ministries involved in the two policy-areas.
Radon (222Rn) is a radioactive, noble insoluble gas with a half-life of 3.8 days. It belongs to the uranium (238U) decay chain where radon is formed from radium (226Ra). Uranium and radium are built ...into mineral structures or are, for example, adsorbed on the surface of clay minerals, limonite or organic material. When radon is formed by radioactive decay from radium, parts of it enter the pores of rocks and soils and are transported by diffusive or advective forces in the pores. The transport rate depends on the permeability and water content in the pores (Nazaroff 1992).
We report the discovery of a remarkable Ly
α
emitting galaxy at
z
= 7.2782, JADES-GS+53.16746−27.7720 (shortened to JADES-GS-z7-LA), with rest-frame equivalent width, EW
0
(Ly
α
) = 388.0 ± 88.8 Å ...and UV magnitude −17.0. The spectroscopic redshift is confirmed via rest-frame optical lines O
II
, H
β
and O
III
in its JWST/NIRSpec Micro-Shutter Assembly (MSA) spectrum. The Ly
α
line is detected in both lower resolution (
R
∼ 100) PRISM as well as medium resolution (
R
∼ 1000)
G
140
M
grating spectra. The line spread function-deconvolved Ly
α
full width at half maximum in the grating is 383.9 ± 56.2 km s
−1
and the Ly
α
velocity offset compared to the systemic redshift is 113.3 ± 80.0 km s
−1
, indicative of very little neutral gas or dust within the galaxy. We estimate the Ly
α
escape fraction to be > 70%. JADES-GS-z7-LA has a O
III
/O
II
ratio (O32) of 11.1 ± 2.2 and a (O
III
+ O
II
)/H
β
ratio (R23) of 11.2 ± 2.6, consistent with low metallicity and high ionization parameters. Deep NIRCam imaging also revealed a close companion source (separated by 0.23″), which exhibits similar photometry to that of JADES-GS-z7-LA, with a photometric excess in the
F
410
M
NIRCam image consistent with O
III
+ H
β
emission at the same redshift. The spectral energy distribution of JADES-GS-z7-LA indicates a “bursty” star formation history, with a low stellar mass of ≈10
7
M
⊙
. Assuming that the Ly
α
transmission through the intergalactic medium is the same as its measured escape fraction, an ionized region of size > 1.5 pMpc is needed to explain the high Ly
α
EW and low velocity offset compared to systemic seen in JADES-GS-z7-LA. Owing to its UV-faintness, we show that it is incapable of single-handedly ionizing a region large enough to explain its Ly
α
emission. Therefore, we suggest that JADES-GS-z7-LA (and possibly the companion source) may be a part of a larger overdensity, presenting direct evidence of overlapping ionized bubbles at
z
> 7.
The Nordic countries lost their 'great power' status in peacekeeping after the end of the cold war. This article asks whether they have succeeded in establishing a new model of cooperation that will ...enable them to regain it. The analysis shows that such a model has been established, but that it remains uncertain whether the Nordics have the collective will to exploit its potential. The article concludes that the Nordics at a minimum would have to establish civil-military rapid reaction deployment packages to reassert themselves as peace operations pace-setters.
Since 1991, a number of European satellites have acquired data of the Earth’s surface for environmental monitoring. In general, a satellite will orbit the Earth in about 1½ hours and it takes 35 days ...before an ERS or ENVISAT satellite repeats radar scanning of the same position. For younger generations of satellites, such as RADARSAT and TERRA, the scanning repeat interval has decreased to 24 and 11 days, respectively, so that hundreds of radar scenes of the same place, produced over the past c. 20 years, are now available.
We present rest-frame optical data of the compact
z
= 5.55 galaxy GS_3073 obtained using the integral field spectroscopy mode of the Near-InfraRed Spectrograph on board the
James Webb
Space ...Telescope. The galaxy’s prominent broad components in several hydrogen and helium lines (though absent in the forbidden lines) and v detection of a large equivalent width of He
II
λ
4686, EW(He
II
) ∼20 Å, unambiguously identify it as an active galactic nucleus (AGN). We measured a gas phase metallicity of
Z
gas
/
Z
⊙
∼0.21
−0.04
+0.08
, which is lower than what has been inferred for both more luminous AGN at a similar redshift and lower redshift AGN. We empirically show that classical emission line ratio diagnostic diagrams cannot be used to distinguish between the primary ionisation source (AGN or star formation) for systems with such low metallicity, though different diagnostic diagrams involving He
II
λ
4686 prove very useful, independent of metallicity. We measured the central black hole mass to be log(
M
BH
/
M
⊙
)∼8.2 ± 0.4 based on the luminosity and width of the broad line region of the H
α
emission. While this places GS_3073 at the lower end of known high-redshift black hole masses, it still appears to be overly massive when compared to its host galaxy’s mass properties. We detected an outflow with a projected velocity ≳700 km s
−1
and inferred an ionised gas mass outflow rate of about 100
M
⊙
yr
−1
, suggesting that one billion years after the Big Bang, GS_3073 is able to enrich the intergalactic medium with metals.
We present emission-line ratios from a sample of 27 Lyman-break galaxies from
z
∼ 5.5 − 9.5 with −17.0 <
M
1500
< −20.4, measured from ultra-deep JWST/NIRSpec multi-object spectroscopy from the ...JWST Advanced Deep Extragalactic Survey (JADES). We used a combination of 28 h deep PRISM/CLEAR and 7 h deep
G
395
M
/
F
290
LP
observations to measure, or place strong constraints on, ratios of widely studied rest-frame optical emission lines including H
α
, H
β
, O
II
λλ
3726, 3729, Ne
III
λ
3869, O
III
λ
4959, O
III
λ
5007, O
I
λ
6300, N
II
λ
6583, and S
II
λλ
6716, 6731 in individual
z
> 5.5 spectra. We find that the emission-line ratios exhibited by these
z
∼ 5.5 − 9.5 galaxies occupy clearly distinct regions of line-ratio space compared to typical
z
∼ 0 − 3 galaxies, instead being more consistent with extreme populations of lower-redshift galaxies. This is best illustrated by the O
III
/O
II
ratio, tracing interstellar medium (ISM) ionisation, in which we observe more than half of our sample to have O
III
/O
II
> 10. Our high signal-to-noise spectra reveal more than an order of magnitude of scatter in line ratios such as O
II
/H
β
and O
III
/O
II
, indicating significant diversity in the ISM conditions within the sample. We find no convincing detections of N
II
λ
6583 in our sample, either in individual galaxies, or a stack of all
G
395
M
/
F
290
LP
spectra. The emission-line ratios observed in our sample are generally consistent with galaxies with extremely high ionisation parameters (log
U
∼ −1.5), and a range of metallicities spanning from ∼0.1 ×
Z
⊙
to higher than ∼0.3 ×
Z
⊙
, suggesting we are probing low-metallicity systems undergoing periods of rapid star formation, driving strong radiation fields. These results highlight the value of deep observations in constraining the properties of individual galaxies, and hence probing diversity within galaxy population.
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